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Abstracts of the 234th AAS Meeting (St. Louis, MO)

American Astronomical Society June, 2019

101 — Kavli Foundation Lecture: during the perihelion passage of sungrazing C/2012 S1 (ISON) in November 2013 are presented Key Outstanding Questions in and compared with earlier measurements made Formation and How to of Kreutz C/2011 W3 (Lovejoy). Comet ISON was an object, probably Answer Them, Alice Shapley entering the for the first time. Strong (UCLA) evidence was found for a radical change in the polarization properties once the tail particles ap- 101.01 — Key Outstanding Questions in Galaxy proached within 10 solar radii of center. Above Formation and How to Answer Them this apparent threshold, the polarization properties of Comet ISON appeared very similar to those seen Alice E. Shapley1 previously for Comet Lovejoy, with high positive 1 UCLA (Los Angeles, California, United States) polarization, and a broad negative branch reaching out to an inversion point between 40-50 degrees. Understanding the formation and evolution of galax- Below 10 solar radii the polarization levels drop ies remains one of the great challenges of mod- dramatically; an effect not seen for Comet Lovejoy. ern cosmology. Key outstanding questions include: We conclude that radiation processes close to the What are the physical processes driving the forma- Sun, and possibly starting as far out as 0.25 AU, are tion of in individual ? How do galaxies responsible for the high levels of polarizations seen exchange matter and energy with their intergalac- in both , and that the sublimation of olivines tic environments? How do the impressive variety and pyroxenes is responsible for the precipitous of galactic structures that we observe today assem- drop in Comet ISON’s polarization below 10 solar ble? How do supermassive black holes affect the radii. evolution of their host galaxies? And how do large- scale structures of galaxies assemble across cosmic 102.02 — Earth At Mars time? I will address these important questions in galaxy formation using new results from powerful Michael L. Cobb1; Samantha Hasler1 ground-based and space-based facilities. I will also 1 Southeast Missouri State Univ. (Cape Girardeau, Missouri, look ahead to future progress with upcoming facili- United States) ties. With its current chemical makeup, Earth would freeze solid if placed at Mars’ . This research 102 — The Solar System Poster explores the possibility of an Earth like main- Session taining liquid water in an orbit like Mars. We used the Global Circulation Model software (Mod- 102.01 — Changing linear polarization properties elE) provided by the Goddard Institute for Space in the dust tail of comet C/2012 S1 (ISON) Studies to reposition Earth into the orbit of Mars. We then increase the amount of greenhouse gasses, pri- 2,1 William T. Thompson marily CO2 , in the atmosphere in an attempt to keep 1 NASA/GSFC (Greenbelt, Maryland, United States) parts of the planet from freezing solid. 2 ADNET Systems, Inc (Lanham, Maryland, United States)

Polarization measurements made with the STEREO/SECCHI COR1 and COR2 coronagraphs

1 102.03 — Carbonyl sulfide (OCS): Detection in two 2 UC Berkeley (Berkeley, California, United States) Oort cloud comets and upper-limits in two -family comets. We establish one step along a technical route to achieving cm/s scale accuracy for astronomical spec- 1 1,2 1 Mohammad Saki ; Erika L. Gibb ; Nathan Roth ; trographs over long time scales, which is critical for 2 3 Michael A. DiSanti ; Neil Dello Russo ; Ronald the characterization of earth sized and 3 4 Vervack ; Hideyo Kawakita measurement of cosmic redshift drift over . Us- 1 University of Missouri St. Louis (Saint Louis, Missouri, United ing a new method called “crossfading” for exter- States) nally dispersed interferometers (EDI) to get highly 2 Goddard Center for , NASA GSFC (Greenbelt, Mary- robust spectra, we have recently demonstrated a fac- land, United States) tor of 1000x reduction in the net shift of an EDI mea- 3 Johns Hopkings University, Applied Physics Lab (Laurel, Mary- sured ThAr line to a deliberate simulated wavelength land, United States) translation of the detector. This 1000x gain in dis- 4 Division of Science, Kyoto Sangyo University (Kyoto, Japan) perser stability can be combined with conventional stability gains afforded by fiber scramblers, vacuum Comets are thought to retain volatiles from the time tanks, and thermal control, to provide an additional of their formation; therefore, characterizing their 2 to 3 orders of magnitude reduction in the net PSF composition should provide insights into the con- shift drift. Crossfading combines high and low delay ditions present in the early solar system. Chemi- process signals using strategic weightings to cancel cal diversity has been noted among comets based on the net reaction to a wavelength drift of the detec- measurements at all wavelengths, including near-IR tor. This can be applied by deploying interferome- studies of parent volatiles. Of these molecules, OCS ters having a stepped mirror that produces two si- is particularly underrepresented in parent volatile multaneous delays, or can be applied to a single de- studies, having been targeted in only a small subset lay that overlaps the spectral response of the ordi- of comets (four OCCs so far). Newer instruments, nary spectrum, and for that case all time scale drifts such as the high-resolution, near-infrared iSHELL are mitigated. Crossfading also mitigates increases spectrograph at the NASA-IRTF on Maunakea, HI, in PSF width and asymmetric distortions. with its large spectral grasp and active M-band guid- ing capabilities, now enable routine sampling of OCS 103.02 — Characterization of Teledyne emissions near 4.9 μm along with other molecules, HAWAII-4RG-15 Infrared Detector Arrays thus we will be able to begin establishing statistics for the OCS content of comets. We targeted OCS in Klaus W. Hodapp1; Donald Hall1; Shane Jacobson1; comets 46P/Wirtanen, 21P/Giacobini–Zinner, and Mickie Hirata2; Markus Loose3; Majid Zandian4 C/2015 ER61 in 2017-2018 using iSHELL, as well as 1 Univ. of Hawaii (Hilo, Hawaii, United States) in C/2002 T7 (LINEAR) using CSHELL in 2004. We 2 Washington University in St. Louis (St. Louis, Missouri, United will present production rates and mixing ratios (with States) 3 respect to H2O) of OCS for these comets and will Markury Scientific (Thousand Oaks, California, United States) place our results in the context of comets measured 4 Teledyne Imaging Sensors (Camarillo, California, United States) to date. This work was supported by the NASA Earth and Space Science Fellowship, Solar System Work- With funding from NSF, the University of Hawaii In- ings, Solar System Observations, and Astrobiology stitute for Astronomy, in partnership with Teledyne Programs, and NSF Solar and Planetary Research Imaging Sensors, LLC, have, over the past decade, Grants. developed the HAWAII-4RG-15 near infrared detec- tor arrays with a cut-off wavelength of 2.5 micro- meters. The ”R” in the name indicates the presence 103 — Instrumentation: Ground of reference pixels, the ”G” stands for guide-window Based or Airborne & Computation mode, and the ”15” indicates the pixel size in micro- meters. These devices are usually abbreviated as Poster Session H4RG-15. The H4RG-15 detector arrays can operate with up 103.01 — A 1000x Stabler Spectrograph using an to 64 output amplifiers, but in our testing program, Interferometer with Crossfaded Delays they were operated by a single Teledyne SIDECAR ASIC with 32 signal channels. In addition to the David John Erskine1; Eric Linder2 frame of 4 rows and columns of reference pixels that 1 LLNL (Livermore, California, United States)

2 the older H2RG devices are using, the H4RG-15 pro- be implemented at both telescopes. Using materials vides reference pixels that can be read out inter- and resources available in the Astronomical Instru- leaved with the IR-sensitive science pixels. In our mentation Laboratory at Southern Connecticut State testing, we routinely used the interleaved reference University, an optical system has been developed to pixels, leading to a full-frame read-out time of 5.4 s. work toward this goal but outfitting the first tele- As part of the development program, Teledyne scope in this way. The light from the telescope is col- had produced three near-science-grade detector ar- limated and directed toward a reflective diffraction rays with two different passivation processes. One of grating. This is then re-imaged using a second lens these, referred to as PV1 here, turned out to be clearly and directed onto the pixels of the photon detector. superior with respect to persistence effects. These optical components have been placed inside an The telescope tests of the best (PV1) device were aluminum housing and can be mounted to the tele- done using the ULB-Cam test system restricted to the scope for test observations. A status report will be J and H bands. These tests showed that under con- given on the observations so far. If this can be repli- ditions of low electronic pickup noise, the use of the cated at the other telescope, the signal-to-noise ratio interleaved reference pixels does not offer an advan- achievable with the instrument could be improved tage over the use of the frame reference pixels. Most by a factor of 2.8. importantly, the telescope tests with standard dither- ing data acquisition showed no noticeable detector 103.04 — The Next Generation GBT persistence in the broad J and H filters. 1 1 The laboratory tests showed only minimal, short Natalie Butterfield ; William P. Armentrout ; Amber 1 1 1 duration persistence on the PV1 device, and moder- Bonsall ; David T. Frayer ; Frank D. Ghigo ; Tapasi 1 1 1 ate persistence on the PV2 devices. For both flavors Ghosh ; Felix J. Lockman ; Ryan S. Lynch ; Ronald 1 1 of detector material, localized persistence near bad J. Maddalena ; Anthony Howard Minter ; Larry 1 1 1 pixel areas was noted and my be caused by internal Morgan ; Karen L. O’Neil ; Andrew Seymour ; Joy 1 stress of the detector material. Nicole Skipper 1 The detector arrays show non-linear photometric Green Bank Observatory (Green Bank, West Virginia, United response near the saturation level due to the changes States) in photodiode capacitance with remaining bias volt- age. This non-linearity can be fitted with a polyno- The Green Bank Telescope (GBT) is the US astro- mial and corrected for. nomical community’s only open-skies, large single- dish radio telescope operating from decimeter to mil- limeter wavelengths. Since its inception, the GBT 103.03 — An Optical System for Multi-wavelength has been an excellent platform for developing and Intensity Interferometry with the Southern deploying new technology in support of a broad Connecticut Stellar Interferometer range of science, including fundamental physics, the Matthew Dever1; Elliott Horch1 transient radio sky, multi-messenger astronomy, 1 Physics, Southern Connecticut State University (New Haven, formation, cosmology, , and the Connecticut, United States) search for life beyond Earth. The Green Bank Ob- servatory (GBO) intends to enhance the capabilities The Southern Connecticut Stellar Interferometer is of the GBT in support of the US scientific commu- an astronomical intensity interferometer consisting nity. Several of these small to mid-scale projects will of two telescopes. Each is currently equipped with include: 1) A growth in the GBT’s radio camera pro- a single-photon avalanche diode (SPAD) detector, gram, 2) Using new digital technology to increase in- and an ultra-fast timing module correlates counts be- stantaneous bandwidth and mitigate the impact of tween both photon detectors. The interferometer has radio frequency interference (RFI), 3) Developing the previously demonstrated intensity correlations us- most sensitive radio receivers, 4) A data archive and ing the 1-pixel SPADs and extremely narrow band scientific tool-kit for large-area surveys, 5) Precision pass filters but was limited in the amount of light that telescope control, 6) Enhancing radio quiet zones, could be collected, and therefore the signal-to-noise and 7) Advanced monitor and control systems. This ratio that could be achieved. SCSU’s recent acqui- poster will discuss these upcoming projects in more sition of an 8-pixel SPAD detector has allowed for a detail and will describe how the GBO plans to imple- new possibility: a different wavelength of light could ment these exciting new capabilities. be directed towards each of the 8 pixels of the detec- tor, thus conducting 8 independent intensity inter- ferometry experiments at the same time, if this could

3 103.05 — The 100m Green Bank Telescope history of assembly of these most massive ob- jects; Karen L. O’Neil1; Will Armentrout1; Amber Bonsall1; Natalie Butterfield1; David T. Frayer1; Frank D. Ghigo1; • Long-baseline very high angular resolution Tapasi Ghosh1; Felix J. Lockman1; Ryan S. Lynch1; studies of active galactic nucleii, disks Ronald J. Maddalena1; Anthony Howard Minter1; Larry around black holes, and other phenomena. Morgan1; Christopher J. Salter1; Andrew Seymour1; Joy Nicole Skipper1 • Studying atomic and molecular gas in the Milky 1 Green Bank Observatory (Green Bank, West Virginia, United Way’s central molecular zone and the Fermi States) Bubble wind; • Measuring the molecular content of galaxies The 100-m, filled aperture, Green Bank Telescope op- near and far, to understand how the gas content erates well between 100 MHz and the atmospheric relates to the formation and evolution of galax- cutoff at 116 GHz, is equipped with state of theare ies. receivers and detectors, and is located in a region that provides terrain shielding and legal protection from interfering sources. The GBT observes 85% of the en- 103.06 — A Fast Poisson Solver with Vacuum tire celestial sphere, and can track an object for the Boundary Conditions in 3D Cylindrical entire time that it is at least 5 degrees above the hori- Coordinates zon. It has the ability to switch between diverse in- Woong-Tae Kim1; Sanghyuk Moon1; Eve C. Ostriker2 struments in its focal plane in just a few minutes, and 1 Seoul National Univ. (Seoul) can be operated remotely. 2 Princeton University (Princeton, New Jersey, United States) The GBT offers “open skies” access for the best peer-reviewed projects and is a training ground for In modelling self-gravitating, rotating disks such as students, something which is increasingly absent massive circumnuclear and protoplanetary disks, it from remote astronomical facilities. It can also be is desirable to employ a fully three-dimensional Pois- used for very long baseline interferometry both with son solver in a cylindrical geometry subject to the telescopes in Europe and those in the western US, open boundary conditions. We develop an accurate and is prime location for bi-static radar studies from and efficient method for such a solver that works transmitters at the Goldstone and Arecibo facilities. in Cartesian, uniform cylindrical, and logarithmic Current high profile science on the GBT in the next cylindrical coordinates. Our method consists of two few years includes: parts: an interior solver and a boundary solver. The interior solver adopts an eigenfunction expansion • Bi-static radar studies of objects in the solar sys- method together with a tridiagonal matrix solver to tem allowing accurate orbital predic- solve the Poisson equation subject to the zero bound- tions; ary condition. The boundary solver employs James’s • Spectroscopy of interstellar molecules with an method with the discrete Green’s function in order to emphasis on organic chemistry, discovering calculate the boundary potential due to the screen- new molecules and understanding their forma- ing charges required to keep the zero boundary con- tion mechanisms; dition for the interior solver. A full computation of gravitational potential requires running the in- • Wide-field mapping of molecular clouds with a terior solver twice and the boundary solver once. high spatial dynamic range to reveal the condi- We perform various tests to check that our solver tions for ; is second-order accurate and exhibits good parallel performance. • Studies of pulsars and other compact objects, in- cluding searches for new pulsars and long term monitoring of pulsars for the detection of gravi- 103.07 — Astronomical Data Mining with NRAO tational radiation; NINE and UWI Trinidad 1 2 2 • Studies of low surface-brightness 21cm HI emis- Brian R. Kent ; Shirin Haque ; Jason D. Renwick ; Alexander Fortenberry3; Brandon Rajkumar2; Ariel sion around galaxies to understand their forma- 2 4 1 tion and evolution; Chitan ; Anja Fourie ; Lyndele Von Schill 1 NRAO (Charlottesville, Virginia, United States) • Making high resolution maps of the Sunyaev- 2 University of the West Indies (St. Augustine, Trinidad and To- Zeldovich effect in galaxy clusters to show the bago)

4 3 University of the Virgin Islands (St. Thomas, Virgin Islands routines and pre-reduced data which is supplied by (U.S.)) the national (and university) telescope facilities. If 4 South African Radio Astronomy Observatory (Cape Town, South flaws exist in the routines or data, or if the instrumen- Africa) tation limits are reached within the data, there is an increasing probability that fact will not be realized We present work from the NRAO NINE - the Na- prior to the data’s publication, resulting in the pub- tional and International Non-traditional Exchange lication of potentially erroneous results. A second, program. NINE aims to broaden participation in and equally important, consequence is that the na- radio astronomy and data mining among a diverse tional facilities will have an increasing difficulty find- group of nations interested in software, hardware, ing knowledgeable staff to create the required data and education development. Workshops at the reduction routines and data products. University of the West Indies at St. Augustine in Observatories are where textbook theories jump Trinidad and Tobago utilized Raspberry Pi single- into action. Training the next generation of as- board computers to introduce students to astronom- tronomers how to not only interpret data, but push ical computing, data mining, and imaging from the the limits of what is possible with current telescopes NRAO VLA Sky Survey (VLASS). With this low-cost is critical for the advancement of astronomical re- computing solution, we can use Python to manipu- search. With commitment to and investment in ob- late images and catalogs as participants make their servatory training programs, the state of our profes- first foray into multi-wavelength data mining. The sion will be strengthened for the next generation of NRAO NINE Program aims to establish active hub scientists and engineers. Here we look at three as- institutions so that participants can further expand pects of the necessary training: [1] telescope training, their skill sets - in the case of UWI the Trinidad Ra- [2] professional advancement, and [3] flexible instru- dio Astronomy Community (TRAC) was established. ment and software experimentation at observatories. TRAC will expand upon educational opportunities in radio astronomy and computing for UWI and the 104.02 — Cal-Bridge: Engaging Underrepresented Trinidad community. Students in Physics and Astronomy Alexander L. Rudolph1; Carol E. Hood2; Aaron J. 104 — Education & History Poster Romanowsky3; Bruce Schumm4; Tammy A. Smecker- Session Hane5 1 Cal Poly Pomona (Pomona, California, United States) 2 104.01 — The Role of Observatories in CSU San Bernardino (San Bernardino, California, United States) 3 Professional Astronomy Training San José State Univ. (San José, California, United States) 4 UC Santa Cruz (Santa Cruz, California, United States) 1 1 1 Karen L. O’Neil ; Will Armentrout ; Amber Bonsall ; 5 UC Irvine (Irvine, California, United States) Natalie Butterfield1; David T. Frayer1; Frank D. Ghigo1; Tapasi Ghosh1; Felix J. Lockman1; Ryan S. Lynch1; We describe the Cal-Bridge program, which has the Ronald J. Maddalena1; Anthony Howard Minter1; Larry mission of increasing participation of groups tradi- Morgan1; Christopher J. Salter1; Andrew Seymour1; Joy tionally underrepresented in physics and astronomy Nicole Skipper1; Sue Ann Heatherly1 through scholarships, significant mentoring, profes- 1 Green Bank Observatory (Green Bank, West Virginia, United sional development, and summer research opportu- States) nities, creating a national impact on their numbers successfully pursuing a PhD in the field. Now in As we transition further into the era of “big data as- its fifth , the Cal-Bridge program is a CSU-UC tronomy,” observatories which have traditionally op- Bridge program comprised of physics and astron- erated as training beds for the country’s future as- omy faculty from 9 University of California (UC), tronomers are being crowded out. They are, nev- 16 California State University (CSU), and more than ertheless, essential in part as training sites for pro- 30 California Community College (CCC) campuses fessional astronomers. The result of this is felt in a throughout California. Cal-Bridge provides mentor- number of ways. First, as the pool of astronomers ing and professional development experiences over with detailed instrumentation knowledge decreases, the last two years of undergraduate and first year of the probability of a given astronomer knowing an in- graduate school to students from this diverse net- strument expert in a given field also decreases. Asa work of higher education institutions. Cal-Bridge result, astronomers become extremely dependent on Scholars benefit from substantial financial support, the quality and accuracy of canned data reduction intensive, joint mentoring by CSU and UC faculty,

5 professional development workshops, and exposure is freely available online so that others may build to research opportunities at the participating UC their own (and modify the code, if they wish). campuses. In addition, they are given summer re- search opportunities through the Cal-Bridge sum- 104.04 — From Clouds to the Stars: the History of mer research program (formerly known as CAM- the Magdalena Ridge Observatory Interferometer PARE). A subset of CAMPARE scholars participate 1 in a program called CHAMP (CAMPARE-HERA As- Ifan Payne 1 tronomy Minority Partnership) in collaboration with NM Tech/MRO (Socorro, New Mexico, United States) the HERA radio telescope consortium. In the first five years, 59 Cal-Bridge Scholars have been selected, This paper presents the history of the development including 34 Latinos, 7 African-Americans and 25 of the Magdlena Ridge Observatory Interferometer women (15 of the 25 women are from underrep- which started with the cloud studies carried out on resented minority groups). Forty-four (44) of the Magdalena Ridge in South Central New Mexico dur- 59 Cal-Bridge Scholars are first-generation college ing the 1930’s. By the 1960’s these studies had grown students. In the first 4 years, 27 of 34 Cal-Bridge to such an extent that they warranted the creation of Scholars have begun or will be attending PhD pro- the Langmuir Atmospheric Laboratory - named for grams in physics or astronomy at top PhD programs eponymous Nobel laureat. Although Langmuir had nationally. The others are attending Master’s-to- never worked in the Magdalena mountains the labo- PhD Bridge programs, Master’s Programs in physics ratory named in his honor was in 1975 was the recip- or astronomy, or in one case, teaching high school ient of the residue of his estate. physics. Five (5) scholars have won NSF Gradu- However, other pioneers of science did work on ate Research Fellowships and three more received Magdalena Ridge, including Charles Moore who as- an Honorable Mention in the first 3 years of the cended in a balloon into the heart of a thundercloud program. Funding for these programs is provided and Stirling Colgate who in 1973 oversaw the estab- by NSF-DUE SSTEM Grants #1356133 and #1741863, lishment of the double telescope Joint Observatory NSF-AST PAARE Grant #1559559, and NSF AST for Cometary Research (JOCR) and in the following MSIP Grant #1564352. year established a digital supernovae telescope on the Ridge. The existence of this astronomy observatory on 104.03 — Orchestar: Teaching the Magdalena Ridge led in 1995 to the gift to New Mex- Color/ Relation through Sound ico Tech of a declassified 2.4-meter primary mirror, Soley Hyman1; Allyson Bieryla1; Daniel Davis2; Wanda originally intended for space surveillance. In turn Diaz Merced3 this led to the design of a 3-element optical inter- 1 Center for | Harvard & Smithsonian (Cambridge, ferometer to be installed on what by now had been Massachusetts, United States) named Magdalena Ridge Observatory. By the year 2 Harvard Natural Sciences Lecture Demonstrations, Harvard 2004, following the signing of a memorandum of University (Cambridge, Massachusetts, United States) agreement with the University of Cambridge in 2002, 3 Office of Astronomy for Development, South African Astronomi- the 3-element array had been redesigned as an array cal Observatory (Cape Town, South Africa) of 10 x 1.4-meter optical telescopes to be the first of the the generation of sparse array optical interferom- The relation between color and temperature is one eters. of the fundamental concepts of an introductory as- It is suggested that in terms of relative resolution tronomy course. However, for non-visual learn- and sensitivity the Magdalena Ridge Observatory In- ers, the association – which is typically taught with terferometer (MROI) will arguably be the most pow- visual aids – can be difficult to make. Using the erful optical telescope on earth; with even greater process of ”sonification,” an Arduino-based device resolution than the Hubble Space Telescope (HST) has been developed at Harvard University to con- and also greater than that of the three much hyped vert color to sound with an RGB color sensor and 30-meter class telescopes that are currently in de- MIDI board. The device, known as Orchestar, is velopment (ELT, TMT, GMT). The sensitivity of the able to sonify both reflected and transmitted light MROI also far exceeds (by a factor of 10 to 100 times) and is intended to be used as a tool for teaching the that of other high resolution interferometers such as color/temperature relation, both in a laboratory set- CHARA, NPOI and the European VLTI. ting and on a telescope. The documentation and code for Orchestar, which costs around $90 to build,

6 105 — Extrasolar Poster 105.03 — Linking the properties of protoplanetary disks and their host stars in the Taurus region Session Dallar Diana Babaian1; Luca Ricci1; Ilaria Pascucci2; 105.01 — Imaging the Interaction between Planets Andrea Isella3 and Young Disks with the ngVLA 1 Physics and Astronomy, California State University, Northridge (Burbank, California, United States) 1 1 2 Sarah Kelley Harter ; Luca Ricci ; Zhaohuan Zhu ; 2 LPL University of Arizona (Tucson, Arizona, United States) 2 Shangjia Zhang 3 Rice University (Houston, Texas, United States) 1 Physics and Astronomy, California State University Northridge (Ventura, California, United States) Protoplanetary disks are dense regions of gas and 2 University of Las Vegas (Las Vegas, Nevada, United States) dust rotating around a young . As the name suggests, protoplanetary disks are where plan- The recent discovery of thousands of protoplanetary ets form. These disks can also serve as accretion ma- disks and exoplanets has revealed that planet for- terial for the young central star. In this project we mation is a very efficient process in nature. There aim to study about 100 protoplanetary disks in the have been several theories to describe the many steps Taurus-Auriga young star forming region. The main along this process, but it remains difficult to dis- focus of our study is the relationships between the cover planets surrounding young stars. Thanks to spectral index, fluxes at mm-wavelengths and stel- its unprecedented angular resolution and sensitivity lar properties, as well as the correlation between the at wavelengths where the emission from the circum- of the central star and the mass of dust in the stellar material is optically thin, the future ngVLA . Disk are inferred us- telescope has the potential to transform our under- ing previous flux observations in 0.89 mm and 1.33 standing of planet formation. In this presentation I mm wavelengths, as well as recent observations at a will highlight the unprecedented imaging capabili- wavelength of 3 mm using The Combined Array for ties of the ngVLA using theoretical models of proto- Research in Millimeter-wave Astronomy (CARMA). planetary disks. These images will help shed light This study will allow us to refine scaling laws linking on how planets interact with disks and young stars, disk and stellar properties, and shed light on the ori- as well as on the properties of forming exoplanetary gin of some of the key scaling laws recently observed systems. from the known population of exoplanets. 105.02 — A Survey of the Habitability of TESS 105.04 — Direct Detection of CO in CI Tau b: Planet Candidates Support for Hot Start Formation Paul Bonney1 Christopher M. Johns-Krull1; Laura Flagg1; Larissa 1 Physics, University of Arkansas (Fayetteville, Arkansas, United Nofi2; Joe Llama2; Lisa A. Prato2; Kendall Sullivan3; States) Daniel Thomas Jaffe3; Gregory N. Mace3 The Transiting Survey Satellite (TESS) has 1 Rice Univ. (Houston, Texas, United States) so far discovered a multitude of potentially habitable 2 Lowell Observatory (Flagstaff, Arizona, United States) planet candidates. The next step in confirming the 3 UT Austin (Austin, Texas, United States) habitability of these exoplanets will be spectroscopic observations by the next generation of telescopes. We analyze high resolution IR spectra of CI Tau, In an effort to prioritize candidates for these obser- the host star of one of the few young planet candi- vations, I have calculated the Earth Similarity In- dates amenable to such observations. We confirm dex (Schulze-Makuch, D. et al., 2011) for each of the the planet’s existence with a direct detection of CO planet candidates identified by TESS that are within in the planet’s atmosphere. We determine a mass of the habitable zones of their host stars. As TESS data 11.6 Mjup based on the amplitude of the planet’s ra- is based on transit observations and not radial veloc- dial velocity variations. We estimate the planet’s flux ity measurements, the of the planets used in contrast with its host star to obtain an absolute mag- the calculations is obtained using the mass-radius re- nitude estimate for the planet of 8.17 in the K band. lationship created by Ning, B. et al. (2018) which in This magnitude implies the planet formed via a ”hot turn is based on data taken from the Kepler mission. start” formation mechanism. This makes CI Tau b Overall, 3 were found to have a global ESI greater the youngest confirmed exoplanet as well as the first than 0.8, indicating an Earth-like planet, though 11 exoplanet around a T Tauri star with a directly deter- had global ESIs between 0.7, the ESI of Mars and 0.8. mined, model-independent, dynamical mass.

7 105.05 — Formation of Satellites Around the Outer 106 — Division Planets of the Trappist-1 System (SPD), Poster Session I Christopher R. Fuse1 1 Rollins College (Oviedo, Florida, United States) 106.01 — Multi-line diagnostics of the coronal magnetic field with DKIST The Trappist-1 system (Gillon et al. 2017) is a com- pact configuration of seven Earth-like planets orbit- Gabriel Dima1; Thomas A. Schad1 ing a M-type dwarf star. The presence of can- 1 National Solar Observatory (Makawao, Hawaii, United States) not be confirmed in the transit data. Orbital param- eter instabilities in the Trappist-1 system are known Full-stokes polarimetric observations of multiple and the timescales of these instabilities have been de- coronal emission lines can in principle be used to termined (Burgasser & Mamajerk 2017). Previous infer the vector magnetic field in the solar corona work by Allen, Becker, & Fuse (2018) found that some assuming the emission is all coming from a single Trappist-1 planets may be able to retain a single satel- location in space. The Fe XIII line pair at 10747 / lite through at least the duration of the planetary in- 10798 Å has already been identified as a prime can- stability. The current study examines the formation didate for multi-line inversions; although such mea- and stability of satellites around the outer planets surements are sensitive to uncertainties and biases Trappist-1f, g, and h. disks are simulated by that must be carefully assessed. That said, this tech- distributing 100 bodies, each with mass 5.26 x 1018 nique may have additional utility when expanded kg randomly within 10% - 90% of the exoplanet’s Hill to other multi-line observations planned for the Na- sphere. Utilizing N-body simulations, the planets tional Science Foundation’s Daniel K Inouye Solar and theoretical moons were tracked for 500 kyrs, al- Telescope (DKIST). This work investigates, in partic- lowing for gravitational interactions and mergers. ular, the use of the Fe XIII 10747 / Si X 14301 Å line pair, and its benefits for probing the magnetic condi- 105.06 — Dust Evolution in the Late Stages of tions in cooler coronal loops formed near 1.4 MK. We Planet Forming Disks discuss the advantages and limitations of the Fe XIII / Si X line pair as well as possible observing scenar- Joshua Garrett1; Luca Ricci1; Carey Louise2; Andrea ios with the DL-NIRSP and Cryo-NIRSP instruments Isella3 on the DKIST. 1 Physics, California State University,Northridge (Santa Clarita, California, United States) 106.02 — Multiscale Helicity Condensation and 2 California State University, Los Angeles (Los Angeles, California, Filament Channel Formation United States) 3 Rice University (Houston, Texas, United States) C. Richard DeVore1; Spiro K. Antiochos1 1 NASA GSFC (Greenbelt, Maryland, United States) We study the properties of dust in disks to constrain models of planet formation. We analyze the spectral Solar eruptive events ranging from small-scale jets index for the dust continuum emission at millime- to global-scale coronal mass ejections are associ- ter wavelengths for 24 young disks in the Upper Sco ated with filaments and their underlying filament- star forming region. We do this by combining data channel magnetic structures. In previous work, taken with the ALMA telescope at wavelengths of we have demonstrated that sheared-arcade filament 2.87 mm and 0.88 mm. Since the age of this region is channels can be formed via the process of helicity ∼ 5 - 10 Myr, these results can constrain the proper- condensation. Magnetic twist, representing helicity, ties of small solids in disks at the end of their lifetime. is transported across unipolar regions in response to We examine whether pebble trapping, which is key reconnection induced by small-scale, close-packed, to planet formation, happens only in much younger surface flows (e.g., the granulation or supergranu- disks or if it is efficient all the way towards the end lation) that possess a vortical component of motion. of the disk life cycle. If the latter is true, planetesi- The small-scale twists induced by the flows inverse- mals could still form despite the low gas in cascade to the largest scales and boundaries of the the disk at the end of its life cycle. In the case of the unipolar regions, i.e., to the polarity inversion lines opposite scenario, our results would indicate that ra- (PILs). If the flows have a preferred sense of rota- dial drift takes over the dynamical evolution of dust tion, clockwise or counter, they inject a net helicity towards the end of the disk lifetime. into the magnetic field, as well as transport it so that it condenses into filament channels at the PILs. We

8 now have examined how the helicity condensation visibility of umbra-to-umbra loops is new evidence mechanism is modified when the small-scale flows that magnetoconvetion drives solar-stellar coronal have no preferred sense of rotation, and large-scale heating: evidently, the strong umbral field at both flows are solely responsible for introducing nethe- ends quenches the magnetoconvection and hence the licity into the corona. On the Sun, differential ro- heating. Broadly, our results indicate that depend- tation is well-known to be a prodigious generator ing on the field strength in both feet, the photo- of helicity. Our new simulation results show that a spheric feet of a on any convective star large-scale shear flow produces structure with large- can either engender or quench coronal heating in the scale magnetic twist, but this twist concentrates near body of the loop. the PILs to form filament channels only when small- This work was supported by funding from the He- scale vortical flows also are present. We conclude liophysics Division of NASA’s Science Mission Di- that the key role of the vortical flows is to transport rectorate, from NASA’s Postdoctoral Program, and the injected net helicity and condense it at the PILs. from the Austrian Science Fund. The results have The source of the net helicity, on the other hand, can been published in The Astrophysical Journal Letters be flows at any scale. We refer to this extended con- (Tiwari, S. K., Thalmann, J. K., Panesar, N. K., Moore, cept as multiscale helicity condensation: it is a more R. L., & Winebarger, A. R. 2017, ApJ Letters, 843:L20). general, hence more robust, explanation for the for- mation of filament channels on the Sun. Our work 106.04 — Revisiting Taylor relaxation was supported by NASA’s H-ISFM, H-SR, and LWS 1 2 TR&T programs. Anthony R. Yeates ; Alexander Russell ; Gunnar Hornig2; Long Chen1 1 106.03 — Invisibility of Solar Active Region Durham University (Cambridge, Massachusetts, United States) 2 Umbra-to-Umbra Coronal Loops: New Evidence Division of Mathematics, University of Dundee (Dundee, United that Magnetoconvection Drives Solar-Stellar Kingdom) Coronal Heating Turbulent magnetic relaxation is an important candi- Ronald L. Moore1; Sanjiv Tiwari2; Julia Thalmann3; date mechanism for coronal heating and some types Navdeep Panesar4; Amy Winebarger5 of . By developing turbulence that recon- 1 Center for Space and Aeronomic Research (CSPAR), Uni- nects the magnetic field throughout a large volume, versity of Alabama in Huntsville (Huntsville, Alabama, United States) magnetic fields can spontaneously self-organize into 2 Lockheed Martin Solar Astrophysics Laboratory, Lockheed Martin simpler lower-energy configurations. We are using (Palo Alto, California, United States) resistive MHD simulations to probe this relaxation 3 University of Graz (Graz, Austria) process, in particular to test whether a linear force- 4 Lockheed Martin Solar Astrophysics Laboratory, Lockheed Martin free equilibrium is reached. Such an end state would (Palo Alto, California, United States) be predicted if one were to assume the classic Tay- 5 and Planetary Science Office ST13, NASA Marshall lor hypothesis: that the only constraints on the relax- Space Flight Center (Huntsville, Alabama, United States) ation come from conservation of total magnetic flux and helicity. In fact, a linear force-free state is not How magnetic energy is injected and released in the reached in our simulations, despite the conservation solar corona, keeping it heated to several million of these total quantities. Instead, the end state is bet- degrees, remains elusive. The corona is shaped by ter characterised as a state of (locally) uniform field- the magnetic field that fills it and the heating ofthe line helicity. corona generally increases with increasing strength of the field. For each of two bipolar solar active re- 106.05 — Characteristics of ephemeral coronal gions having one or more in each of the two holes main opposite-polarity domains of magnetic flux, from comparison of a nonlinear force-free model of Andrew Inglis1; Rachel O’Connor3; W. Dean Pesnell2; the active region’s three-dimensional coronal mag- Michael S. Kirk1; Nishu Karna4 netic field to observed extreme-ultraviolet coronal 1 The Catholic University of America (Greenbelt, Maryland, United loops, we find that (1) umbra-to-umbra loops, de- States) spite being rooted in the strongest magnetic flux 2 NASA/GSFC (Greenbelt, Maryland, United States) at both ends, are invisible, and (2) the brightest 3 Smith College (Northampton, Massachusetts, United States) loops have one foot in a umbra or penum- 4 Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- bra and the other foot in another sunspot’s penum- sachusetts, United States) bra or in unipolar or mixed-polarity . The in-

9 Small-scale ephemeral coronal holes may be a recur- cadence and integration times needed to resolve in- ring feature on the solar disk, but have received com- dividual Alfven-wave oscillations, as have been seen paratively little attention. These events are character- with CoMP. ized by compact structure and short total lifetimes, substantially less than a solar disk crossing. Follow- 106.07 — Constraining CME Mass in HI-1 ing a search of the time period 2010 - 2015 using At- 1 1 mospheric Imaging Assembly EUV image data from Phillip Hess ; Robin Colaninno 1 the Solar Dynamics Observatory, we present analy- Space Science Division, U.S. Naval Research Laboratory (Wash- sis of four of the clearest examples of the ephemeral ington, District of Columbia, United States) phenomenon. The properties of each Mass is an important parameter in both the physi- event are characterized, including their total life- cal processes which govern CME motion and is di- time, growth and decay rates, and areas. The mag- rectly linked to CME observations, as most remote netic properties of these events are also determined sensing measurements of a CME are white-light im- using Heliospheric Magnetic Imager data. These ages where intensity is correlated with density. As ephemeral coronal holes possess common charac- such, mass is both a crucial parameter to measure teristics, experiencing rapid initial growth of up to and one of the few that can be studied directly. Most 2 ∼3000 Mm / hr, while the decay phases are typi- attempts to determine masses from remote sensing cally more gradual. Like conventional coronal holes, data have focused on coronagraph data, where the the mean magnetic field in each ephemeral coronal CME is bright and still a roughly self-similarly ex- hole displays a consistent polarity, with mean fields panding flux rope that has undergone few dynamic generally < 10 G. No evidence of a corresponding changes since the initial eruption. However, to un- signature is seen in data at 1AU. Further derstand the flux rope evolution once the CME be- study is needed to determine whether ephemeral gins to interact with the upstream solar wind and coronal holes are under-reported events or a truly determine how it may change in the , it is rare phenomenon. necessary to probe the data and constrain the mass at higher heights. Attempts to extend the coronagraph 106.06 — Forward Models of Off-Limb Emission methods and study the mass at higher heliographic Lines in Solar Coronal Holes distances have been difficult given the low signal to noise ratio of CME observations in the STEREO Chris Gilbert1; Steven R. Cranmer1 1 SECCHI HI-1 FOV. This study uses improved im- Astrophysical and Planetary Sciences, University of Colorado age processing techniques to better isolate the ejecta (Boulder, Colorado, United States) mass from the background. Obtaining this signal There is debate in the solar community regarding the without resorting to running-difference techniques mechanism by which the corona is heated to mil- reduces the amount of useful signal lost due to im- lions of degrees. Alfvén waves, driven by granula- age processing while still reducing the unwanted tion in the and propagating upwards contribution from stars and other background fea- to dissipate in the corona, are one of several ideas tures. By comparing the obtained masses with both for the source of the thermal energy. Observations COR2 measurements as well as in-situ densities we of off-limb spectral lines are in theory able to con- can better understand the challenges in determining strain some properties of these waves (e.g., ampli- mass farther away from the Sun and quantify the tudes and phase speeds) as a function of heliocentric systematic error such an approach introduces. Di- altitude, but in practice the interpretation of these rectly studying more local evolution of the mass in- measurements is difficult due to the optically-thin side the CME, we can directly address the degree to nature of the corona. In this work, a forward model which the CME evolves non-uniformly and how mo- (GHOSTS) is developed and refined so that it can mentum is transferred between the CME and the up- be used to generate realistic simulated observations stream solar wind. of these lines. Recent improvements to the model include the addition of resonantly scattered light 106.08 — Adding RESTful web services to the and the self-consistent calculation of frozen-in non- VSO: How to write Data Providers in Python equilibrium states. Early results indicate Edmund Mansky1 that the non-thermal widths of these lines seem to 1 be significantly broadened by the presence of the so- NASA/GSFC (Greenbelt, Maryland, United States) lar wind, even as close to the Sun as a few tenths of Adding support for RESTful web services to the VSO a . We also aim to put constraints on the codebase is described. The ability to query Data

10 Providers as RESTful web services generalizes the effects. Since, the total energy must be conserved, it VSO so both SOAP and REST data transfer tech- is possible that the reduced wave energy is deposited niques are supported. The requirements of adding in the plasma. Further experiments are necessary queries to remote RESTful services from a multi- to confirm if this wave energy contributes to plasma threaded Perl application is detailed. Examples of heating. RESTful Data Providers written in Python, using the Flask and Django frameworks are provided. The 106.10 — A Total Observing Tool to two primary Data Providers illustrated are the new Advance Coronal Heating Knowledge and Bolster Parker Solar Probe and the existing EUNIS re-written Authentic STEM Undergraduate Research as a Python Data Provider. Automatic validation of Experiences the RESTful service, in both Perl and Python is ex- 2 1 amined. Use of unit tests in Python and load test- Noah Kirkland Stolz ; Norton B. Orange 1 ing using Locust is also detailed. The steps needed OrangeWave Innovative Sciences (Charleston, North Carolina, to write new RESTful Data Providers in Python are United States) 2 presented. Rensselaer Polytechnic Institute (Troy, New York, United States) A formidable solar physics challenge is describing 106.09 — Alfvén waves propagating in an the magnetic-to-radiative energy coupling of the inhomogeneous plasma similar to those in coronal Sun’s atmosphere. Total solar eclipses provide a holes rare opportunity to advance our knowledge of so- 1 2 1 lar atmospheric energy redistribution processes, as Sayak Bose ; Troy Carter ; Michael Hahn ; Shreekrishna the structure, distribution, and dynamics of coronal Tripathi2; Steve Vincena2; Daniel Wolf Savin1 1 magnetic fields, as well as the emission spectrum of Columbia Astrophysics Laboratory, Columbia University (New the can be directly observed. We built York city, New York, United States) 2 the Solar Eclipse Observing Package (SEOP) as a tool Physics and Astronomy, University of California, Los Angeles for pc control of linear polarizing, white light, and (Los Angeles, California, United States) flash spectrum digital camera systems to advance Alfvén speed gradients in directions parallel and our knowledge of coronal heating by observing the perpendicular to the ambient magnetic field in coro- August 21st 2017 total solar eclipse. Last minute nal holes are thought to aid dissipation of wave en- cloud cover unfortunately kept our expedition from ergy and thus contribute to coronal heating. We have observing totality of this eclipse. However, during studied Alfvén wave propagation under conditions the months, and up to the last minutes leading to similar to coronal holes in the Large Plasma Device its totality, the computer, engineering, and coronal located at University of California, Los Angeles. The physics science behind our team’s SEOP, imaging energy of Alfvén waves propagating in the presence systems, and scientific objectives were disseminated of an Alfvén speed gradient perpendicular to the am- through a number of educational engagements and bient magnetic field is observed to spread to higher outreach activities. Plans are now underway to ob- serve the next total solar eclipse to cross the conti- k⊥. This spreading of energy is more prominent for nental United States in April 2024. steeper gradients and larger z/λ∥, where z is the dis- Funding Sources: University of the Virgin Islands, tance away from the antenna, and λ∥ is the wave- length parallel to the ambient magnetic field. Our OrangeWave Innovative Science, LLC, St. Thomas initial analysis shows that spreading of wave energy Astronomy Resource Society, and the US Depart- ment of Agriculture. to higher k⊥ may enhance the rate of dissipation of wave energy. However, additional experiments are necessary to confirm plasma heating. Alfvén waves 106.11 — Community Input Solicited for propagating through an Alfvén speed gradient par- Heliophysics Decadal Survey Midterm allel to the ambient magnetic field are observed to Assessment Committee lose five times more energy than they do when prop- Thomas N. Woods1; Robyn Millan2; Arthur Charo3 agating through the same distance in the absence 1 Univ. of Colorado (Boulder, Colorado, United States) of a gradient. This reduction in wave energy is ob- 2 served to increase monotonically with an increase in Dartmouth College (Hanover, New Hampshire, United States) 3 National Academies of Sciences, Engineering, and Medicine λ‖/L퐴,∥, where L퐴,∥ is the scale length of the Alfvén speed gradient parallel to the magnetic field. The (Washington, District of Columbia, United States) cause of this reduction in energy is constrained by The National Academies of Sciences, Engineering, ruling out reflection, mode conversion and nonlinear and Medicine has convened a committee to review

11 the progress towards implementing the 2013 Helio- quality at various points during the alignment to en- physics Decadal Survey, titled Solar and Space Physics: sure that the mechanical tolerances maintain the op- a Science for a Technological Society. This review tical quality of the system so that the instrument will serves as a midterm assessment before the next He- be able to achieve excellent spectral resolution lim- liophysics Decadal Survey committee would begin ited by the spectrograph slit width (λ/Δλ∼250,000), its formulation. This committee is interested to re- and preserve the diffraction limited spatial resolu- ceive input from the heliophysics and tion provided by the telescope and feed optics (0.06” communities about the 2013-2018 progress realiz- at 1 μm). ing the 15 recommendations and applications speci- fied in the 2013 Heliophysics Decadal Survey, about 106.13 — A Makeover for HMI Magnetic Field any suggested actions to optimize the science value Data during 2019-2023, about any suggestions to improve 1 1 1 the process for the next Heliophysics Decadal Sur- Jon Todd Hoeksema ; Yang Liu ; Philip H. Scherrer 1 vey, and about any suggested actions to enhance Stanford Univ. (Stanford, California, United States) all stages of careers for scientists and engineers in HMI, the Helioseismic and Magnetic Imager on the the solar and space physics community. This poster Solar Dynamics Observatory (SDO) has measured will outline the Heliophysics Decadal Survey rec- the Sun’s vector magnetic field nearly every 135 or ommendations and recent progress, and it will also 90 seconds since May 2010. The Stokes parameters summarize the tasks for this midterm assessment are determined from sets of filtergrams every 720 committee. There will be an opportunity to dis- seconds over the full disk. The quality of the im- cuss your inputs with a couple of the Committee ages is remarkably uniform and the measurements members during the AAS/SPD meeting, and web- are reliable for many types of analysis. However, based community-input survey opportunities are an- the inverted and disambiguated magnetic field val- ticipated to be available soon. ues are occasionally incorrect, show small periodic variations with time and spacecraft velocity, or de- 106.12 — Optical Alignment of DL-NIRSP pend in a systematic way on disk position or magni- Spectrograph tude. Estimates of uncertainties in the inversion are Sarah A. Jaeggli1; Tetsu Anan1; Maxim Kramar2; provided for each point, but for some kinds of analy- Haosheng Lin2 sis having a smoother and more uniform time series 1 National Solar Observatory (Pukalani, Hawaii, United States) is necessary. 2 Institute for Astronomy, University of Hawaii (Pukalani, Hawaii, Sources of some errors are well understood and United States) well characterized, but others are not. Statistical and empirical techniques have been developed by the The Diffraction-Limited Near-Infrared Spectropo- HMI Team and others to improve both the calibration larimeter (DL-NIRSP) will be delivered as part of and appearance of the observations, to increase con- the first light instrumentation for the Daniel K. In- sistency, and minimize undesirable variability. Ef- ouye (DKIST) and is currently un- fects addressed include issues related to field inver- dergoing lab integration at the University of Hawai’i sion, disambiguation, sensitivity, optical distortion, Institute for Astronomy’s Advanced Technology Re- instrument characteristics, and systematic errors due search Center on Maui. An off-axis hyperbolic mir- to spacecraft velocity and viewing angle. Some of the ror, with a focal length of 1250 mm, is used as most reliable and affordable corrections are included both collimator and camera in the spectrograph, and in the regular analysis pipeline. Some corrections are makes this system particularly difficult to align. The too compute intensive to implement routinely. For optical axis, or vertex, of the parent surface is lo- others the resulting ’corrections’ depend on assump- cated approximately 260 mm from the center of the tions about the typical behavior of the solar magnetic off-axis section of the mirror, but there is no direct field, so care must be taken when using such results. physical or optical reference for the location and ori- entation of the optical axis. We have made use of 106.14 — Solar Polar Observing vendor data and a coordinate measuring machine (SPOC): A New Age for Solar Observations (CMM) arm to transfer coordinates from the back and perimeter surfaces of the mirror to locate the Lisa Upton1; Thomas Berger2; Nicole Duncan3; Natasha optical axis focus and place the other optical com- Bosanac2 ponents in reference to this mechanical model. In 1 Space Systems Research Corportation (Alexandria, Virginia, coordination, we have conducted tests of the optical United States)

12 2 University of Colorado at Boulder (Boulder, Colorado, United and corona. Realistic high-resolution radiative MHD States) simulations reveal a complex multiscale structuring 3 Ball Aerospace (Boulder, Colorado, United States) and dynamics above the photosphere. We present a detailed study of dynamical links between small- Current observing platforms can only measure the scale magnetic fields generated by local dynamo ac- solar magnetic field over a portion of the Earth- tion and properties of the chromosphere and corona, facing hemisphere, forcing us to rely on solar rota- as well as effects of coherent self-organized magnetic tion to build up fictional “synoptic maps” of the full- structures. In particular, we discuss formation of Sun field over 27-days. The lack of magnetic field coherent structures, eruptive dynamics, and contri- “boundary conditions” over the full Sun represents butions of multi-scale structuring and highly non- a fundamental gap in our ability to accurately model linear dynamics to heating of the chromosphere and the solar coronal magnetic field and solar wind accel- corona. eration. Views restricted to the plane cannot capture the Sun’s polar regions. Observation of the 106.16 — Homologous Coronal Mass Ejections poles from a high latitude vantage point are needed and Their Precursor Phase to advance and constrain the Sun’s polar fields and high latitude flows, which arecru- Suman Dhakal1; Panditi Vemareddy2; Nishu Karna3; Jie cial to understanding the solar activity cycle. Fur- Zhang1 thermore, sustained observation of the Sun’s polar 1 Physics and Astronomy, George Mason University (Fairfax, Vir- regions will enable helioseismology investigations ginia, United States) of the polar subsurface flows, allowing us to probe 2 Indian Institute of Astrophysics (Bengaluru, Karnataka, India) deeper into the mechanisms of the . 3 Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- We propose a novel constellation of small satel- sachusetts, United States) lites called the Solar Polar Observing Constellation (SPOC) that will obtain magnetic field and doppler We present the study of three homologous solar velocity measurements from a solar polar orbit, in- eruptions from the AR 11429. These eruptions oc- cluding nearly direct overhead measurements of the curred at different evolutionary phase of the AR i.e. poles. The SPOC constellation consists of two iden- emergence and decay phase of the magnetic flux. It tical satellites placed into ∼90-degree inclination was a big and complex AR and could be divided into heliocentric using Jupiter gravitational assist two sub-regions, namely north-east (NE) and south- (JGA) trajectories and ion electric propulsion to cir- west (SW). We found that there was continuous in- cularize the orbit at about 0.9 AU. Instrumentation jection of magnetic helicity and energy flux in the includes a compact helioseismic magnetic imager, AR. Further, we observed continuous shearing mo- compact coronagraph, and in-situ solar wind plasma tion of the magnetic flux, converging motion of the measuring instruments. The SPOC mission follows opposite magnetic polarity, and magnetic flux can- the model of “hybrid operational-research” missions cellation in the SW sub-region. We believe that these developed by the CU Space Weather Technology, Re- physical processes were continuously adding helic- search, and Education (SWx-TREC) to enhance util- ity and energy into partially erupted magnetic sys- ity and collaboration by developing critical opera- tem and were responsible for the formation of identi- tional data sources for space weather forecasting that cal erupting structures along the same polarity inver- can also produce exploratory science data. sion line (PIL). A small confined flare was observed, at the left side of SW sub-region, during the pre- 106.15 — 3D Realistic Modeling of Chromospheric cursor phase (PP) of each homologous eruption. It and Coronal Heating and Self-Organization was identified as peak in soft X-ray (SXR) intensity profile, brightening of hot-channel structure (HCS), Irina Kitiashvili1,2; Alan A. Wray1; Alexander G. and appearance of flare ribbon below the HCS. Using Kosovichev3; Viacheslav M. Sadykov3,2; Nagi N. the results of Non Linear Force Free Field (NLFFF) Mansour1 model we studied the magnetic topology of the SW 1 NASA Ames Research Center (Mountain View, California, United sub-region. The magnetic topology of the AR was States) stable and persistent during the evolution of the AR, 2 BAERI (Mountain View, California, United States) therefore flare during the PP was observed around 3 NJIT (Newark, New Jersey, United States) the same location. Our study suggests that the PP- flare facilitate the eruption of magnetic structure, ly- Turbulent magnetoconvection is a primary driver of ing along the SW-PIL, by weakening the overlying the dynamics and structure of the solar atmosphere

13 magnetic . We also think that the contin- two instruments onboard Solar Dynamic Observa- uing flux cancellation along the SW-PIL repeatedly tory (SDO), i.e., the Helioseismic and Magnetic Im- re-produced a twisted magnetic flux rope following ager (HMI) and the Atmospheric Imaging Assembly each eruption. (AIA). We are extending the same calibration methods 106.17 — Three-dimensional Reconstruction of to other instruments, which include: (1) the Inter- CMEs and Observational Constraints of Measured face Region Imaging Spectrograph (IRIS), (2) the So- Parameters lar Optical Telescope (SOT) onboard Hinode, and (3) AIA/HMI. 1 1 1 Eleni Nikou ; Jie Zhang ; Dusan Odstrcil We summarize the modification and optimization 1 Physics, George Mason University (Fairfax, Virginia, United of the methodology and present the results of the States) calibrations. Time variation of the roll angles and the plate scales will be discussed. The results can be This study focuses on the early evolution and propa- used for better coalignment. gation of coronal mass ejections (CMEs) close to the We have also done the calibration between differ- Sun. We are tracking the evolution of both the ejecta ent wavelengths of SOT filtergram data. After the and its shock . We focus on CMEs that were ob- corrections using the calibration results, we can still served during the period 2010-2012 and in this study see some offsets between the different wavelength we present four of them. Events that occurred close images which vary with the position of the observ- to the disc center as viewed from Earth are observed ing region on the solar disk. We attribute this to the as limb events from the two STEREO spacecraft and differing heights of formation associated with each that gives us the opportunity to reconstruct their wavelength band. three dimensional structure. We are using the grad- uated cylindrical shell (GCS) model to fit the ejecta 107.02 — A Statistically-Validated Approach for and the 3D spherical shell model to fit the shock with Flux Emergence Identification white light data from three viewpoints separated by about 90 degree from each other. Thanks to three Derek Lamb1; Emma S. Jones3; Deborah H. Glueck2 viewpoints of observations, we are able to constrain 1 Southwest Research Institute (Boulder, Colorado, United States) parameters like the aspect ratio of the ejecta (cross 2 Department of Pediatrics, University of Colorado School of section size) and its shock (radius) as well as the tilt Medicine (Aurora, Colorado, United States) angle, which we find are difficult to constrain with 3 Department of Biostatistics, University of Colorado Denver, Col- two viewpoints of observations. Being able to con- orado School of Public Health (Aurora, Colorado, United States) straint those parameters can lead to a better under- standing of the morphology and evolution of CMEs We present a new method for automatically identi- and help the prediction of space weather. The ability fying events of magnetic flux emergence in time se- to have accurate predictions is closely related to mon- ries of magnetograms of the sun. Despite their obvi- itoring the Sun from multiple viewpoints, i.e., three ous and striking visual appearance, these events can or more, which implies a need of multi-spacecraft be surprisingly difficult to identify with high speci- mission in the future. ficity and sensitivity. Because of the broad range of spatial and temporal scales across which emergence occurs, as well as a host of physical, geometrical, nu- 107 — iPoster Session: Solar merical, and sometimes operational considerations, Physics Division (SPD), Session I accurate detection has been difficult to implement. In this presentation, we describe our technique, de- 107.01 — Cross calibration for coalignment, veloping a logistic regression model based on thresh- Hinode/SOT, IRIS, and SDO olds of user-defined quantities such as signed and unsigned magnetic flux in a region, the time deriva- Keiji Yoshimura1; Charles Kankelborg1 tive of those quantities, etc. A backward stepwise 1 Montana State University (Bozeman, Montana, United States) approach is used to find the best predictors of mag- netic flux emergence, and the score cutoff chosen to Yoshimura and McKenzie (Solar Physics, vol.290, maximize the paired sensitivity and specificity. The p.2355, 2015) reported the results of the success- final model is evaluated using the area under the ful cross calibration for the coalignments between Receiver-Operator-Characteristic (ROC) curve. We the X-Ray Telescope (XRT) onboard Hinode and describe the performance of the method, highlight-

14 ing events for which a successful detection is made, However, extreme ultraviolet (EUV) and soft x-ray missed, or falsely identified. (SXR) telescopes rarely approach diffraction-limited performance because conventional reflective optics 107.03 — Listening to the Sun of adequate size typically cannot be manufactured to the requisite figure accuracy. Diffractive optics 2 1 W. Dean Pesnell ; Kyle Ingram-Johnson can overcome the angular-resolution limitations of 1 Eleanor Roosevelt High School (Greenbelt, Maryland, United EUV/SXR mirrors. We describe a mission approach States) that employs diffractive optics and small satellites 2 NASA GSFC (Greenbelt, Maryland, United States) flying in formation to form a distributed solar tele- scope operating at EUV wavelengths. How many ways can we explore the Sun? We have images in many wavelengths and squiggly lines of 107.05 — Laboratory measurement of many parameters that we can use to characterize the large-amplitude whistler pulses generated by fast Sun. We learn that the Sun is bright with regions magnetic reconnection that are dark in some wavelengths and bright in oth- ers. But those classifications are both based on vi- Magnus Albert Haw1; Paul M. Bellan1 sion. Sound is another sense to use in exploring solar 1 Applied Physics, Caltech (Pasadena, California, United States) data. Some data, such as the sunspot number or the extreme ultraviolet spectral irradiance, can be easily We present observations of large-amplitude (δB/B sonified. Images are more difficult. A simple raster ∼ 0.01) oblique whistler wave pulses generated by scan is dominated by moving on and off the limb of spontaneous, 3D magnetic reconnection in the Cal- the Sun. Any sonification of the raster scan will con- tech jet experiment. The wave pulses are mea- tain discontinuities at the limbs that mask the infor- sured far from the reconnection location using a mation contained in the image. We propose to sam- multicluster B-dot probe with a tetrahedral arrange- ple the curves with Hilbert curves to reduce those ment, mimicking the formations of the Cluster discontinuities. Hilbert curves are continuous space- and Magnetospheric Multiscale Mission spacecraft. filling curves that map the two-dimensional coordi- These pulses are confirmed to be whistler modes nates of an image onto a linear variable. We have by measurements of the background parameters, investigated using Hilbert curves as ways to sample the wave polarization, and the wave dispersion. and analyze solar images. Reading the image along a The results demonstrate that impulsive reconnection Hilbert curve keeps neighborhoods close together as events can generate large-amplitude oblique whistler the resolution (i.e., the length of the Hilbert curve) in- wave pulses. This provides a new generation mech- creases. It also removes most of the detector size pe- anism for magnetospheric whistler pulses and may riodicities and actually shows the presence of longer- help explain relativistic particle acceleration in other scale features. We shall provide several examples of systems with impulsive magnetic reconnection such sonified solar data, including the sunspot number, as solar flares. a selection of EUV spectral irradiances, an AIA 171 image, and a series of images during a solar flare. 107.06 — Radio Propagation Diagnostics of the Inner Heliosphere in the Era of the Parker Solar 107.04 — Ultrahigh-Resolution Imaging of the Probe

Solar Corona using a Distributed Diffractive 1 2 Telescope Adam Kobelski ; Timothy S. Bastian ; Angelos Vourlidas3 Douglas M. Rabin1; Adrian N. Daw1; Kevin Denis1; 1 West Virginia University (Morgantown, West Virginia, United Farzad Kamalabadi2; James A. Klimchuk1 States) 1 NASA Goddard Space Flight Center (Greenbelt, Maryland, 2 National Radio Astronomy Observatory (Charlottesville, Virginia, United States) United States) 2 Electrical and Computer Engineering, University of Illinois at 3 JHU/APL (Laurel, Maryland, United States) Urbana-Champaign (Urbana, Illinois, United States) The solar wind offers and extraordinary laboratory Several observational and theoretical considerations for studying turbulence, turbulent dissipation, and suggest that energy is often released in the solar heating. The Parker Solar Probe (PSP) was launched corona on small spatial scales of order 100 km. It in August 2018 to study these and other important has been a longstanding goal of solar physics to processes in the inner heliosphere. One type of ob- subject this hypothesis to direct observational test. servation that will complement those of PSP are ra-

15 dio propagation measurements of solar wind turbu- propagating disturbances observed in the solar lence in the outer corona and the inner heliosphere. corona, frequently associated with coronal mass ejec- This type of observation can provide measurements tions and flares. They appear as faint, extended of the angular broadening of distant spatially co- structures propagating from a source region across herent background sources that transilluminate the the structured solar corona. Since their discovery, foreground solar wind plasma. This well-known over two hundred papers discussing their proper- technique can be used to measure the spatial spec- ties, causes and physical nature have been published. trum of electron density inhomogeneities in the solar However, despite this their fundamental properties wind on scales of 100s of meters to 10s of kilometers and the physics of their interactions with other so- inside of 10-15 solar radii over a wide range of posi- lar phenomena are still not understood. To fur- tion angles. ther the understanding of EUV waves, we have con- Here we report the results of a pilot study of back- structed the Automated Wave Analysis and REduc- ground sources using the Jansky Very Large Array tion (AWARE) algorithm for the measurement of (JVLA) in summer 2015. Unlike previous studies of EUV waves. AWARE is implemented in two stages. this kind, the JVLA’s much greater sensitivity allows In the first stage, we use a new type of running dif- fainter and more numerous sources to be used as ference image, the running difference persistence im- probes of the foreground medium. We observed 11 age, which enables the efficient isolation of propagat- background sources in 16 sessions at apparent ra- ing, brightening wavefronts as they propagate across dial distances of 2-7 solar radii. We confirm previ- the corona. In the second stage, AWARE detects the ous findings: that the spectrum is flatter than Kol- presence of a wavefront, and measures the distance, mogorov and that is highly anisotropic. Unlike pre- velocity and acceleration of that wavefront across vious studies we find breaks into steeper spectra for the Sun. The fit of propagation models to the wave some sources on short spatial scales, suggestive of a progress isolated in the first stage is achieved using transition to dissipation. the Random Sample and Consensus (RANSAC) al- Looking forward, we describe observations gorithm. AWARE is tested against simulations of planned in August 2019 in support of the third PSP EUV wave propagation, and is applied to measure perihelion passage (35.7 solar radii). The VLA will EUV waves in observational data from the Atmo- be used to observe the corona and inner heliosphere spheric Imaging Assembly (AIA). We also comment along ∼70 pierce points <10 solar radii. These on unavoidable systematic errors that bias the esti- observations will not only provide global context mation of wavefront velocity and acceleration. In ad- about the state of the inner heliosphere at time of dition, the full AWARE software suite comes with a perihelion passage, they will also baseline key solar package that creates simulations of waves propagat- wind parameters that can be compared directly ing across the disk from arbitrary starting points. with PSP measurements. These include turbulence level, spectral index, degree of anisotropy, and the orientation of the magnetic field. The PSP measure- 108 — iPoster Session: Dust & Star ments will, in turn, provide measurements that will Formation validate key assumptions made in interpreting the radio data. 108.01 — Differential abundance techniques applied to iron in two mid-F stars 107.07 — AWARE: An algorithm for the automated characterization of EUV waves in the solar Charles R. Cowley1; Kutluay Yuce2 atmosphere 1 Univ. of Michigan (Ann Arbor, Michigan, United States) 2 Dept of Astronomy and Space Sciences, Faculty of Science, Uni- 1 4 1 Jack Ireland ; Andrew Inglis ; Albert Y. Shih ; Steven versity of Ankara (Ankara, TR-06100, Ankara, Turkey) Christe1; Stuart Mumford3; Laura A. Hayes1,5; Barbara J. Thompson1; V. Keith Hughitt2 We explore and extend the technique of precision 1 NASA Goddard Spaceflight Center (Greenbelt, Maryland, United abundance differences to the mid-F domain, deriv- States) ing iron abundance differences between θ Scl (F5 2 NIH (Bethesda, Maryland, United States) V), and (F5 IV-V) using UVESPOP spectra 3 University of Sheffield (Sheffield, United Kingdom) (Bagnulo, et al. ESO Messenger 114, 2003). The 4 CUA / NASA GSFC (Greenbelt, Maryland, United States) spectra have resolving power of 80,000. S/N ratios 5 NPP Fellow (Greenbelt, Maryland, United States) measurements are in agreement with Bagnulo et al. (300-500). We report results for 35 Fe I and 24 Fe II Extreme ultraviolet (EUV) waves are large-scale

16 weak and moderate lines (4.3-90mÅ), measured in- high-resolution spectra from the Hubble Space Tele- dependently by the authors, using Voigt (CRC), and scope Imaging Spectrograph (HST/STIS), the God- Gaussian (KY) profiles. The mean difference (CRC- dard High Resolution Spectrograph (GHRS), and KY) for the Fe I lines was 1.26mÅ ± 0.25mÅ (se). the Very Large Telescope Ultraviolet Visible Echelle Abundances were based on Atlas9 models (Castelli Spectrograph (VLT/UVES). In order to perform an and Kurucz, IAU Symp. 210, 2003), Te=6550 for abundance analysis for Sirius A that does not assume both stars, log(g)=3.71 & 4.2, Vt=2 & 1.5 km/s, re- LTE, we have employed the model atmo- spectively for Procyon and θ Scl. In principle, pair- sphere code to compute 1-D non-LTE models and wise abundance ratios are independent of gf val- spectra. These models treat 194 species, 34976 levels ues, but for stronger lines saturation must be pre- and 600676 transitions in non-LTE for several ions of cisely taken into account. We explore departures all elements from to lead except Se, Br, Kr, from the weak-line approximation. For example, the Sb, Te, I, Xe, Pt, Au, Tc, and Pm to further constrain 26.2 mÅ line Fe I 5247.05 in Procyon would be larger Sirius A’s elemental abundances. by a factor of 1.28 (0.11 dex) if it were unsaturated. We have thus far compared our non-LTE abun- Discrepancies of this nature depend on the state of dance results with literature values for 30 elements ionization and excitation of the line and especially and find six elements (N, Na, Cu, Mo, Ba, Os) have the microturbulence. We examine the effect of as- abundances which differ by more than 2 standard suming that the average of the logarithms of abun- deviations (∼0.6 dex or more) from literature values. dances may/should be used in place of the logarithm These results appear to differ from previous work of the averages. For example, the average abun- for three reasons: (1) the latest oscillator strengths dance logarithms for our 24 Fe II lines in Procyon from Kurucz (2014) may differ significantly (2 to 10 is -4.5820, and in θ Scl is -4.6108. The difference is times) from earlier values for specific lines and (2) 0.0288. If we take abundance quotients (not logs) for non-LTE models show enhanced ionization of trace each line pair (θ Scl/Procyon) the average is 1.09214, species relative to LTE which depletes these species whose logarithm is 0.0383. The difference is 0.0383- and elevates the abundance needed to match the ob- 0.0288=0.0095–not trivial for precision abundances. served spectrum, and (3) non-LTE departure coeffi- We use abundance quotients, and then take logs. The cient values for specific lines may different signifi- mean abundance differences of log(θ Scl/Procyon) cantly from unity. We also find our model for Sirius for Fe I and Fe II respectively were +0.0528 ± 0.0086 A provides a good match to the observed spectral en- (se), 0.0511 (sd) and +0.0383 ± 0.0189 (se). 0.0927 ergy distribution in absolute units between 100 nm to (sd). The standard errors (se) are in the 0.01-0.02 dex 1 cm based on recent observations obtained by White range. There is no significant difference in the iron et al. (2019) with ALMA, GBT, and the VLA. abundance of these two stars. 108.03 — The SOFIA-FORCAST imaging survey 108.02 — A massively non-LTE model atmosphere toward Giant HII regions of the Galaxy for Sirius A Wanggi Lim1; James M. De Buizer1; James Radomski1 1 Jason P. Aufdenberg1; Allison Acosta1; Peter SOFIA Science Center (Moffett field, California, United States) Hauschildt2 1 Embry-Riddle Aeronautical Univ. (Daytona Beach, Florida, The massive young stellar objects (MYSOs) crucially United States) affect the ecology of their mother clouds due to the 2 Hamburger Sternwarte (Hamburg, Hamburg, Germany) enormous feedback. Despite of the importance, we barely understand massive star forming mechanisms Elemental abundances in the atmosphere of Sirius since they are rare, typically far at several kpc dis- A reveal a history of nucleosynthesis. Sirius A has tance and deeply embedded in the densest parts of tightly constrained fundamental parameters due to molecular clouds. Giant HII (GHII) regions in Milky its orbit with Sirius B, a measured interferometric Way are perfect laboratories to study the massive star diameter, and a precise . Its slow rotation formation since they are well known active star form- and apparent lack of atmospheric convection sug- ing regions dominated by forming massive stars. In gest one-dimensional model atmospheres should be this poster, we present the current status of SOFIA- a good approximation. Recent abundance analy- FORCAST 20 and 37 micron imaging survey toward ses of Sirius A from Landstreet (2011) and Cow- the GHII regions of Milky Way. We also utilize the ley et al. (2016) have employed local thermody- archival data from near-infrared to centimeter wave- namic equilibrium (LTE) models in comparison to length regimes in order to understand the physical

17 properties and the relative formation histories of in- throughput of ∼100 cm2 deg2, compared to 0.09 cm2 dividual proto-stars as well as the porto-clusters. The deg2 for XRISM/XARM/Hitomi and 50 cm2 deg2 analyses imply that the studied GHII regions possess for Athena. An instrument can be constructed that MYSOs at their earliest evolutionary stages while en- fits within the size/mass/cost envelope of a Small- tire areas show widely ranged life span of proto- Sat and has a lifetime up to 60 days. This is short for clusters. These analyses toward all known GHII re- a satellite, but even a 14- science mission is the gions will provide us revolutionary point of views to equivalent of 3,629 sounding rocket flights, which is massive star formation mechanisms. the only alternative for obtaining these data until the Athena era begins in 2031+. We show some of the 108.04 — Angular momentum in bipolar outflows: science questions that can be addressed by this mis- dynamical evolutionary model sion. Jesus Alejandro Lopez-Vazquez1; Jorge Canto2; Susana Lizano1 109 — iPoster Session: Extrasolar 1 Instituto de Radioastronomia y Astrofisica, UNAM (Morelia, Planets Michoacan, Mexico) 2 Instituto de Astronomia, UNAM (Mexico, Ciudad de Mexico, 109.01 — A Gaussian Process Regression Reveals Mexico) No Evidence for Planets Orbiting Kapteyn’s Star We model molecular outflows produced by the Jinbiao Ji1; Hallie Fausey1; Anna Bortle1; Sarah E. time dependent interaction between a stellar wind Dodson-Robinson1; John Gizis1 and a rotating cloud envelope in gravitational col- 1 University of Delaware (Newark, Delaware, United States) lapse, studied by Ulrich. We consider spherical and anisotropic stellar winds. We assume that the bipo- A significant issue with (RV) planet lar outflow is a thin shocked shell, with axial sym- searches is that they are often polluted by signals metry around the cloud rotation axis and obtain the caused by activity on the star’s surface. Stellar ac- mass and momentum fluxes into the shell. We solve tivity can mimic or mask changes in the radial veloci- numerically a set of partial differential equations in ties caused by orbiting planets, resulting in false pos- space and time, and obtain the shape of the shell, the itives. Here we test whether Gaussian process (GP) mass surface density, the velocity field, and the an- regression (e.g. Haywood et al. 2014) can distinguish gular momentum of the material in the shell. We find star rotation from wobbles due to planets. We ex- that there is a critical value of the ratio between the amine the RV and Hα data for Kapteyn’s star, which wind and the accretion flow momentum rates β that has reported planets Kapteyn b and c with periods allows the shell to expand. As expected, the elon- 48.6 and 121.5 days, respectively (Anglada-Escude gation of the shells increase with the stellar wind et al. 2014). Based on the Hα observations, which anisotropy. In our models, the rotation velocity of trace magnetic activity in M dwarfs, Robertson et al. the shell is the order to 0.1–0.2 km s−1, a factor of 5– (2015) argued that Kapteyn b was an alias of the rota- 10 lower than the values measured in several sources. tion. Here we use a quasiperiodic GP kernel to model We compare our models with those of Wilkin and rotation in the RV and Hα data jointly, requiring that Stahler for early evolutionary times and find that our their period and decorrelation timescale be the same. shells have comparable sizes at the pole, although we From this model, we construct residual RV datasets use different boundary conditions at the equator. after subtracting off realizations of the GP rotation model. We find no evidence that Kapteyn’s star hosts 108.05 — XQCSAT: A High-Resolution any planets, as there were no significant signals that Spectroscopic Study of Hot Gas in the Halo and remained in the residual data. We suggest that the periodic signals of the previously reported planets are both products of the star’s rotation. Dan McCammon1; Philip Kaaret2 1 Univ. of Wisconsin (Madison, Wisconsin, United States) 109.02 — A Search for Exoplanets in High 2 University of Iowa (Iowa City, Iowa, United States) Open Clusters Using a Large-Scale We have completed a design feasibility study for Photometric Algorithm a SmallSat carrying an array of microcalorimeter Ashini Modi1; Michael Fitzgerald2; Saeed Salimpour2 detectors optimized for the 100 – 1000 eV spectral 1 Caddo Magnet (Shreveport, Louisiana, United States) range. It will have an energy resolution ∼6 eV and a

18 2 Edith Cowan Institute for Educational Research. (Perth, New Earth-like planets also provides insight into the fu- South Wales, Australia) ture climate of our own planet. A database of cli- mate models based on different orbital parameters, A is a group of stars in close proximity to solar irradiance and atmospheric composition will each other that are gravitationally bound. Open clus- provide a valuable resource to the astrobiology com- ters can contain about 100 to 1,000 stars. Stars in open munity in support of future detections of exoplan- clusters have the same origin, as they all formed from ets with masses, sizes, and compositions similar to the same . Open clusters are also composed of Earth. Due to its user-friendly interface to a re- stars with the same age. These conditions make open search grade 3-D climate model code, the Educa- clusters suitable for exoplanet formation, for new tional Global Climate Model (EdGCM) was selected star harbor a lot of dust and gas in their surround- to perform a limited number of simulated models us- ings. Gas and dust from young stars are two main ing the land configuration of Earth, but with vary- factors in the process of new planet formation. Al- ing amounts of greenhouse gases, orbital parame- though all stars once existed in a cluster, no exoplan- ters, and axial tilts. It is found that the EdGCM is ca- ets have been discovered in open clusters. The pur- pable of simulating 3-D climate models for hypothet- pose of this project is to observe whether exoplan- ical Earth-like planets for a limited number of cases, ets can form and remain in open clusters with high with several important restrictions on the initial con- solar metallicity, to further the understanding about ditions. planetary formation and evolution. If we search for exoplanets in high-metallicity open clusters, then we should see a higher number of planets than we 110 — iPoster Session: Cosmology would expect in normal stars. For my research I have and Related Topics operated multiple 0.4m optical telescopes affiliated with the las cumbres global telescope network (LCO) 110.01 — The Role of NED in Identifying EM and a 0.4m telescope located at the University of Dal- Counterparts to GW events las. With these telescopes I have taken observations of 3 open clusters; NGC 6791, NGC 2112, and NGC David O. Cook1; Joseph M. Mazzarella1; Rick Ebert1; 6253. We hypothesize that the high metallicity of the Marion Schmitz1; Jeffery D. Jacobson1; Scott Terek1; stars in the open clusters may provide elements and Xiuqin Wu1; George Helou1 materials needed to form exoplanets. My research 1 Caltech/IPAC (Pasadena, California, United States) has led to the discovery of 7 interesting transits that The detection of gravitational waves (GWs) has may be those of potential Hot-. However, opened a new window into the Universe by enabling further observatins and data analysis needs to be direct studies of mergers of massive, compact ob- conducted on these stars to confirm any current find- jects. Some of the largest impacts on our understand- ings. 75 potential eclipsing binaries were also dis- ing of these events will come when combining the covered in this research and we hypothesize that this GW data with their electromagnetic (EM) counter- is because of the relatively young age of the stars in parts. However, due to the large area (> 100 deg2) these clusters, causing them to still be gravitationally localization of LIGO events, identifying their correct bound to eachother. EM counterparts is no small feat and is akin to find- ing a needle in a haystack. This search is and will 109.03 — An Investigation of 3-D Climate Patterns continue to be difficult task due to the large (>100 on Hypothetical Earth-like Planets deg2) localization of LIGO events. To overcome R. Mark Elowitz1 this challenge several teams used a galaxy-targeted 1 University of North Dakota (Grand Forks, North Dakota, United approach to successfully locate the EM counter- States) part to the star-neutron star merger event GW170817. In this talk I introduce a new service Studying extreme climate patterns on Earth-like of the NASA/IPAC Extragalactic Database (NED) planets as a function of atmospheric greenhouse that will provide prioritized lists of galaxies located gases, planetary obliquity, , so- within future LIGO 90% probability contours to fa- lar irradiance variations and location within the host cilitate searches for EM counterparts, starting with star’s habitable zone is needed to determine whether the O3 run scheduled to begin in April 2019. I will such planets are habitable for life as we know it. give an overview of the service, as well as an analy- Studying the behavior of climate on hypothetical sis of the local Universe NED galaxy sub-sample and comparisons with other local galaxy lists.

19 110.02 — (withdrawn) 111 — iPoster Plus I: Solar Physics This abstract was withdrawn. Division (SPD), The Corona

110.03 — Strong Gravitational Lenses and Where 111.02 — Mapping low solar corona flow trends to Find Them: Which Method Should We Be via time dependent AIA image processing Using? Gabriel Domingo Muro1; Huw Morgan1 1 1 Shawn Michael Knabel ; Benne Holwerda ; Rebecca 1 Physics, Aberystwyth University (Aberystwyth, Ceredigion, 1 Steele United Kingdom) 1 Physics and Astronomy, University of Louisville (Louisville, Kentucky, United States) The Atmospheric Imaging Assembly/Solar Dynam- ics Observatory (AIA/SDO) has captured high reso- Strong gravitational lenses are cases where a distant lution, continuous ultraviolet images of the Sun since background galaxy is located directly behind a mas- 2010. Applying the Time-Normalized-Optical-Flow sive foreground galaxy, whose gravity causes the (TNOF) image processing technique to AIA Extreme light from the background galaxy to bend around Ultraviolet (177–305 nm) data reveals fine-scale and the foreground galaxy. In addition to being visu- faint plasma motion that are tracked through opti- ally stunning, these rare events are useful laborato- cal flow methods, giving 2-D flow maps. The mo- ries for furthering our understanding of gravity and tions are faint and impossible to analyze without ad- to determine properties, such as the mass, of the vanced processing due to the dominance of the sig- lensing galaxies themselves. The trouble is finding nal range by spatial gradients: these are removed by enough of these strong gravitational lenses for fur- the TNOF process that operates solely in the time do- ther study. The immensity of the catalogs being col- main. lected by state-of-the-art telescopes requires equally The ubiquitous, continuous flows appear to be ori- innovative methods for interpreting that data. We ented in the low corona [1,2]. The Lucas-Kanade op- are interested in three such techniques for identi- tical flow algorithm [3] is currently limited to regions fying strong lenses: mixed spectroscopy, machine- near disk center due to projection effects near the learning, and citizen-science. Spectroscopy involves limb, and is also limited to the higher-signal channels studying the objects’ signatures across the electro- of AIA. To refine the method, synthetic solar image magnetic spectrum and is a tried-and-true, reliable data has been developed with a defined velocity field method. Machine-learning promises to find more and serves as the testing platform to isolate system- and potentially different cases of lensing through atic biases from true flows. Here, we present com- teaching the computer to recognize features of lens- parisons between the robustness of two optical flow ing through visual templates. Citizen-science is a algorithms: Lucas-Kanade, and Horn-Schuncke [4] broad term for the inclusion of science-enthusiasts and their ability to estimate the underlying velocity in the process of analyzing images on a scale too field. A line-integral convolution [5] is used to effec- large to be undertaken by a small team of experts. tively visualize the consistency of flow paths. The For the first time, all three detection techniques have refined system for mapping flow trends is then ap- been used in the same regions of the sky, where the plied to a sample AIA dataset, with the aim of char- Kilo Degree Survey (KiDS) overlaps three regions acterizing the faint moving disturbances that prop- of the Galaxy and Mass Assembly (GAMA) survey. agate, persist, and appear to be the standard solar We have all three catalogs of strong lenses in hand condition in the “quiet sun”. Additionally, the veloc- and plan to analyze the strengths and weaknesses of ity field reveals large-scale flow behavior associated each method. We expect to uncover inherent biases with (i) coronal rotation and (ii) a statistical relation- and advantages to each method in finding a variety ship between velocity relative to the angle of the so- of lensing cases, which will serve as a directory for lar radial-observer vectors. We believe the flow fields selecting the preferred methods to be used in new are closely tied to the underlying coronal magnetic research toward these phenomena based upon the field. characteristics of the target galaxies. With astron- [1] Morgan, H., Druckmller, M. 2014, Solar omy moving into the era of large-scale imaging sur- Physics, Vol. 289. [2] Morgan, H., Hutton, J. veys, we will need to know which of the three tech- 2018, Astrophysical Journal, Vol. 853. [3] Lucas, niques works best for detecting these rare astronom- B., Kanade, T. 1981, Proceedings of Imaging Un- ical events. derstanding Workshop, pg. 121-130 [4] Horn, B., Schunck, B. 1981, Artificial Intelligence, Vol. 17 [5]

20 Cabral, B., Leedom, L. 1993, Proc. of the 20th conf. previously reported dimmings. We investigated the on Computer graphics and interactive techniques, temperature and density evolution of the dimming pg. 263-270 features, as well as the eruptive filament itself. We uncovered large-scale magnetic field connectivity 111.03 — Capturing CMEs in SUVI-ECI data between the conjugate dimmings and remote coro- nal holes where brightenings were observed around 1 Neal E. Hurlburt the time of the eruption. These remote brightenings 1 Lockheed Martin Corp. (Palo Alto, California, United States) are possible precursors of the eruption or manifes- tations of its associated global magnetic reconfigu- The SUVI instrument on GOES-17 (now GOES-West) ration process. These results are significant because spent a month between August and September, 2018 they allow us to use dimmings as tracers to probe the conducting an extended coronal imaging campaign. Sun’s magnetic connectivity and the mechanisms re- Composite images constructed from interleaved im- sponsible for the initiation of space-weather driving age sets that scanned ±4 solar radii across the Sun solar eruptions. every ∼6 minutes were processed to create a con- sistent dataset for analysis. An optical flow method (opflow3d) was applied to this set to estimate veloc- 112 — iPoster Plus II: The Sun, ities of moving features. The results were then com- pared to CMEs detected by the CACTUS algorithm Solar System & Public Policy operating on co-temporal LASCO images. While the peak speeds reported by opflow3d were significantly 112.01 — What is the role of flare ribbon structure lower than the CMEs found further out in the corona on CME speeds? by CACTUS, the time intervals of enhanced motions Brian Welsch2,1; Michael Hencheck2; Maria D. correlate well between the two sets. Here we present Kazachenko1; David Ginsburg2 the data and discuss the processing, analysis and fu- 1 UC-Berkeley (Berkeley, California, United States) ture work. A new set of observations are scheduled 2 University of Wisconsin - Green Bay (Green Bay, Wisconsin, to begin in mid-April. If they begin on time we may United States) report on those results too. Coronal mass ejections (CMEs) are the primary 111.04 — Long-lasting Conjugate Coronal drivers of severe space weather disturbances, but re- Dimmings Produced by a Filament Eruption: main poorly understood. Hence, efforts to character- Implications for Global Magnetic Connectivity ize and predict their dynamics are ongoing. Many CMEs are associated with solar flares, and, in partic- Manan Kocher1,2; Wei Liu1; Cooper Downs3 1 ular, flare ribbons, which are bright bands of strongly Lockheed Martin Solar and Astrophysics Laboratory (San Fran- enhanced emission originating above magnetized ar- cisco, California, United States) 2 eas of the photosphere. As a solar eruption pro- Bay Area Environmental Research Institute (Petaluma, California, gresses, these ribbons typically move across areas United States) 21 3 that contain fluxes of order 10 Mx or more. The Predictive Sciences Inc. (San Diego, California, United States) rate at which the ribbons sweep across photospheric flux is thought to correspond to the rate of coronal Coronal dimmings, typically observed at extreme magnetic reconnection. Previous studies found sig- ultraviolet (EUV) wavelengths, are commonly asso- nificant correlations between CME speeds and the ciated with solar eruptions, such as coronal mass total amount of flux swept by flare ribbons. Here, ejections (CMEs) and eruptive filaments. They of- we investigate relationships between CME speeds fer critical clues to our understanding of the under- and spatial moments of their source-region photo- lying mechanisms and consequences of solar erup- spheric magnetic fields and flare ribbons, including tions. We present a study of an intriguing dim- spatial moments of: (i) magnetic flux in the source ming event associated with a quiescent filament region; (ii) signed and (iii) unsigned magnetic flux eruption on March 6, 2018 observed by SDO/AIA, within ribbon areas; and (iv) binary maps ribbon ar- STEREO/SECCHI, and IRIS. There were notably eas. Our sample consists of N = 75 CMEs in the sigmoid-shaped, conjugate dimmings that appeared SOHO/LASCO CME catalog that were manually as- concurrently in multiple EUV channels, but evolved sociated with flare ribbons identified in SDO/AIA asymmetrically with time. One of the double dim- data. Vector magnetograms obtained by SDO/HMI mings lasted more than two days, which clearly sets were used in our calculations of source-region mag- it apart from the typical lifetime of several hours in

21 netic properties. We confirm prior results that cor- with an admission as to certain shortcomings and relations between CME speeds and total magnetic need for further exploration. It will conclude with an fluxes swept by flare ribbons are statistically signif- invitation for comment and discussion on the critical icant. We also find that spatial moments of ribbon extra-legal factors. magnetic fields are also significantly correlated with CME speeds. 112.03 — Local Weather Conditions and Sky Brightness 112.02 — Navigating the Ownership of Extracted 1 1 1 Parts of Celestial Bodies Vayujeet Gokhale ; Jordan Goins ; Ashley Herdman ; James Tompkins1,2; Emily Wren1; David Caples2 Charles Lee Mudd1 1 Truman State University (Kirksville, Missouri, United States) 1 John Marshall Law School (Chicago, Illinois, United States) 2 Moberly Area Community College (Kirksville, Missouri, United States) Celestial bodies remain free from claims of owner- ship by sovereign nations and their subjects. Yet, Poor and inefficient outdoor lighting has a negative significant debate exists on whether ownership can impact on the environment, and the resulting light be claimed over extracted parts of such celestial bod- pollution greatly hampers our ability to enjoy the ies. Although a mining company cannot claim own- beauty of the night sky and to do astronomy re- ership of the Moon or Mars, could it claim owner- search. The ‘light pollution research group’ at Tru- ship of elements and minerals extracted therefrom? man State University (Kirksville, Missouri) has set An analysis must begin with international space law. up Unihedron sky quality meters at various locations The current paradigm includes five (5) treaties. And, around Kirksville to quantify the sky brightness. In their relevant portions give rise to the very debate at the past year, a weather station, a cloud-sensor, and issue. Consequently, guidance must be sought else- an all-sky-camera have been set up at the Truman where. Perhaps not surprisingly, the tenets and es- State Observatory to monitor the weather conditions tablished principles of maritime law exhibit instruc- and cloud coverage in the Kirksville area. We present tive similarities. results based on data obtained from these sensors. Under the United States and English Com- We correlate the sky brightness measured by the Uni- mon Law system, maritime law established rules hedron light sensors with cloud coverage, humidity, of engagement beyond the borders of individual and temperature. Pictures takes from the all-sky- sovereign nations. In open waters over which camera are used to visually ascertain the changes in no nation or person could claim ownership, mar- the sky brightness as a function of these weather pa- itime jurisprudence established principles of law rameters. Our results indicate that the sky brightness that guided parties for centuries. Given the analogy is greatly affected by even modest amounts of cloud to space and the absence of territorial boundaries, it coverage, whilst the temperature and humidity do serves as a model for space law. not affect sky brightness significantly. We planon In fact, beyond the ownership of elements and repeating this exercise at urban locations (university minerals extracted from celestial objects, these prin- campuses) and dark sky locations (state/national ciples of law can address abandoned spacecraft, parks) in order to quantify the level of sky brightness satellites, and other man-made objects (or fragments and its correlation to local weather conditions. This thereof) occupying various orbits around and be- work is part of our effort to quantify and mitigate yond Earth. Indeed, the research on these histori- the nuisance of light pollution in the Kirksville area. cal principals (based on United States and the En- Apart from data collection and analysis, we have suc- glish Common Law System) give constructs to a pro- cessfully lobbied to obtain close to $10,000 over the posed basis for international law governing owner- past two years to install ‘dark sky reflectors’ (light ship in space. That being said, any proposal will shields) on unfriendly outdoor light fixtures, and to also need to accommodate extra-legal factors such replace the white (5000K) lights with friendlier yel- as principals of scientific research, the policies and low (3000K) lights. We call on amateur and profes- requirements guiding , multi- sional astronomers to act now to save our night skies, disciplinary ethics, and consideration of factors yet and provide an outline for actions to bring about sim- unknown. ilar changes on other campuses and towns. The presentation will address a hint of existing celestial ownership space law and a distinction be- tween three maritime principles. From the most ap- plicable principle, proposed tenets will be revealed

22 113 — Extrasolar Planets ing atmospheric escape is very important from the standpoint of habitability since atmospheric evolu- 113.01 — Lessons Learned and Fascinating Finds tion influences the climate and the fluxes of ionizing from a Manual Vetting of Conflicted KOIs radiation reaching the surface, among other factors. Here we carry out sophisticated 3D multi-species Jeffrey Coughlin1,2 MHD simulations to assess how the atmospheric es- 1 SETI Institute (Mountain View, California, United States) cape rates of the TRAPPIST-1 planets evolve during 2 NASA Ames (Mountain View, California, United States) the passage of an ICME, where the ICME is initial- ized and modeled according to the flare observa- Over the course of the Kepler mission, a total of tions. 9,564 Kepler Objects of Interest (KOIs) were identi- fied via eight KOI catalogs. Each catalog examined 113.03 — Atmospheric Responses to Radiative a different initial set of transiting planet search de- Forcing: Physics and Observability of Close-in tections, and each catalog utilized a different vet- and Highly Eccentric Planets ting procedure to distinguish valid planet candidates from false positives — manual vetting in early cat- Arthur Daniel Adams1; Gregory P. Laughlin1; Sarah alogs, and fully automated vetting in later catalogs Millholland1; William R. Boos3,4; Eric T. Wolf2 tailored for exoplanet occurrence rate studies. As a 1 Astronomy, Yale University (New Haven, Connecticut, United result, many KOIs were vetted multiple times, with States) over 1,400 KOIs having conflicting dispositions, be- 2 University of Colorado, Boulder (Boulder, Colorado, United ing labeled ”planet candidate” in at least one catalog States) and ”false positive” in at least one other. An effort 3 University of California, Berkeley (Berkeley, California, United was undertaken by the Kepler False Positive Working States) Group (FPWG) to manually and individually review 4 Lawrence Berkeley National Laboratory (Berkeley, California, each of these conflicted KOIs, using the latest Kepler United States) data, diagnostics, and follow-up observations avail- able. In this talk, I will present the findings from this The thermal emission of exoplanets contains valu- manual review, which include insights on potential able information about the structures of their atmo- pitfalls in automated vetting, a check on statistical spheres. However, the current quality of observa- planet validation, and possibly overlooked, scientifi- tions allows for only a limited understanding of the cally unique planet candidates and variable stars. physics at play. With this in mind we focus on infrared observables of close-in and eccentric plan- 113.02 — How Flares regulate Atmospheric Losses ets, whose atmospheric responses may be character- from the TRAPPIST-1 planets ized to leading order by the cycles of stellar forcing from their orbits and rotation. We approach model- Chuanfei Dong1; Meng Jin3; Manasvi Lingam2 ing using a range of physical complexities. Firstly, 1 Princeton University (Plainsboro, New Jersey, United States) we demonstrate in a re-assessment of Spitzer or- 2 Harvard-Cfa (Cambridge, Massachusetts, United States) bital phase curves that their shapes in many cases 3 SETI Institute (Mountain View, California, United States) are well fit by a simple thermal model, in compari- son with models of considerably more complexity. Stellar flares are considered an impediment to hab- A few Hot Jupiters show phase offsets counter to itability, especially in the case of close-in exoplan- the expectation of super-rotating winds on a tidally- ets around M-dwarfs since these stars are highly ac- locked planet; we detail the efficacy, feasibility, and tive. In recent times, there has been a growing aware- observable consequences of high planet obliquity ness that coronal mass ejections (CMEs) - sometimes in reproducing these offsets. Finally, we explore termed as stellar storms or superstorms, depending the broad effects of high eccentricity and rotation on the flare energy - associated with stellar flares rate on potentially observable phase variations from pose severe threats to . Inter- ocean-rich worlds, using the capabilities of a fully 3- planetary CMEs (or ICMEs), corresponding to fast- dimensional climate model. moving magnetic clouds, act to impact the plan- ets with significantly high dynamic pressure. Semi- 113.04 — (withdrawn) analytical models imply that planets around active stars (∼1 flare/day) may experience escape rates that This abstract was withdrawn. are 1-3 orders of magnitude higher than those aris- ing from erosion by stellar winds alone. Understand-

23 113.05 — A New Kepler Occurrence Rate Using operations and target selection strategy of space ob- DR25 Completeness and Reliabilty servatories. We are developing a series of numeri- cal simulations to quantify how ground-based radial Steve Bryson1; Jeffrey Coughlin1,2; Natalie Batalha3; 4 6 velocity surveys could boost the detection efficiency Christopher Burke ; Jessie Christiansen ; Susan of forthcoming NASA direct imaging missions such Mullally5 1 as WFIRST, HabEx and LUVOIR. As a first step, we NASA Ames Research Center (Moffett Field, California, United generate synthetic planet systems based on the ob- States) served occurrence rates from multiple planet detec- 2 SETI Institute (Mountain View, California, United States) 3 tion methods. We implement a stability criterion for UC Santa Cruz (Santa Cruz, California, United States) multi-planet systems based on mutual Hill radii sep- 4 MIT (Cambridge, Massachusetts, United States) 5 aration. It is found that naive extrapolation of planet Space Telescope Sciences Institute (Baltimore, Maryland, United occurrence rates results in an unstable high occur- States) 6 rence rate at large semimajor axes. Imposed stability IPAC/Caltech (Pasadena, California, United States) criteria therefore result in a marked suppression of low-mass planets at large semimajor axes compared We present a new occurrence rate estimate based to extrapolated rates. A consequence of tight dynam- on the Kepler DR25 catalog for exoplanets with pe- ical packing, this result has a pronounced impact riod between 50 and 400 days and radius between on planet yield calculations, particularly in the re- 0.75 and 2.5 Earth radii around GK dwarf stars. We gions accessible to both RV and high-contrast imag- make full use of the DR25 completeness and relia- ing measurements. The dynamically self-consistent bility products, introducing a new treatment of vet- occurrence rates that we develop may be incorpo- ting completeness and reliability as realizations of bi- rated as input into joint RV and direct imaging planet nomial processes with variable rates. This approach yield calculations. is robust against the choice of sampling resolution and does not require restricting the sample to high- reliability planet candidates. We use the stellar prop- 114 — Laboratory Astrophysics erties of Berger et. al. 2018 and 2019 which includes -derived stellar radii. This is one of the first Division Meeting (LAD): Bridging occurrence rate estimates to use the reliability data Laboratory & Astrophysics: from DR25, which is a significant factor that impacts occurrence rate calculations. For exoplanets with pe- Molecules and Spitzer I riod and size within 20% of that of Earth, we find lower occurrence rates than those previously pub- 114.01 — LAD Career Prize: At the Interface: lished, partly due to the increased exoplanet radii re- Laboratory and Radio Astronomical Spectroscopy vealed by Gaia data, and partly due to the impact of of Exotic Interstellar Molecules low reliability for small planets near one-year orbits. Lucy M. Ziurys1 1 Univ. of Arizona (Tucson, Arizona, United States) 113.06 — Planet Population Demographics for Radial Velocity and Direct Imaging Yield Observations of molecules in the interstellar medium Calculations (ISM) have shown that the chemistry in space is full of surprises, with the appearance of many unusual, Shannon Dulz1; Peter Plavchan2; Justin R. Crepp1; “non-terrestrial” species. Using high resolution ro- Chris Stark3; Rhonda Morgan4; Stephen Kane5; Patrick tational spectroscopy in the laboratory, combined Newman2; William Matzko2; Gijs Mulders6 with millimeter-wave astronomy, we have pursued 1 Univeristy of Notre Dame (Notre Dame, Indiana, United States) the identification of these exotic molecules in the 2 George Mason University (Fairfax, Virginia, United States) ISM, in particular those containing metals (in the 3 Space Telescope Science Institute (Baltimore, Maryland, United chemists’s sense) or phosphorus. The laboratory States) studies have been conducted with millimeter/sub- 4 NASA/Jet Propulsion Laboratory (Pasadena, California, United mm/THz direct absorption spectrometers, as well States) as a pulsed, Fourier transform microwave/mm-wave 5 University of California, Riverside (Riverside, California, United instrument, all designed and built in the Ziurys States) group. Critical to the laboratory work has been the 6 University of Chicago (Chicago, Illinois, United States) development of synthetic techniques to create the Planet yield calculations are crucial to the science desired molecules, which are typically free radicals.

24 These lab studies have enabled us to identify new unanswered: (a) what is the structure of interstellar magnesium, aluminum, iron and even vanadium- (water) ice (and is it porous)? (b) to what extend does bearing molecules, such an MgCN, AlNC, FeCN, (water) ice aid the earliest stages of planet formation AlOH, and, most recently, VO, typically found in through collisions? (c) how does chemical complex- circumstellar envelopes of evolved stars, along with ity emerge (in the solid state)? In this invited talk I’ll phosphorus-containing species such as CCP. A key very breifly illustrate one example where innvoative to success in this work has been the synergy be- laboratory experiments are enable us to start under- tween the lab studies and observations. Many of the standing these issues, and relate our findings back detections were made at the telescopes of the Ari- to observational data. First I’ll show how we can zona Radio Observatory (ARO) and required sensi- probe the (water) ice porosity using neutron scatter- tive, stable instrumentation, that we implemented. ing techniques, to concurrently elucidate the molec- Also, the molecular identifications were often aided ular structure and mesoscale porosity of the mate- by observing ”non-standard” sources. For exam- rial — and even watch the pores collapse. Second I’ll ple, our pioneering studies of the oxygen-rich enve- show how we can use these same neutron techniques lope of supergiant VY CMa led to the first discov- to explain “why ices stick” and look at what happens eries of circumstellar metal oxides and hydroxides. if we make more “protoplanetary disk” like ices in Our more recent observations have suggested that the laboratory and then collide them — can we build planetary nebulae may hold some interesting molec- planets at all? Finally I’ll illustrate our newest labo- ular secrets. Even more recently, we have teamed ratory development-THz DES (desoprtion emission with solid-state spectroscopists in the investigation spectroscopy) and its potntial to aid our understand- of “presolar” grains extracted from , and ing of COM formation and evolution in star-forming may have found to a facile route to large carbon regions. molecules from SiC destruction. 114.03 — Supersonic Gas Jets as an Interaction 114.02 — Unlocking the star-formation freezer; Medium for Laboratory Photoionized Plasmas showing how laboratory studies are vital in Kyle James Swanson1; Vladimir Ivanov1; Roberto understanding interstellar ices — from SPITZER 1 1 1 and AKARI to the ALMA / JWST era. Mancini ; Daniel C. Mayes ; Nicholas Wong 1 Physics, University of Nevada Reno (Reno, Nevada, United Helen Jane Fraser1 States) 1 Astronomy, The Open University (Milton Keynes, United King- Photoionized plasmas are important for a variety of dom) astrophysical environments such as x-ray binary sys- The Spitzer space telescope revolutionised our view tems, active galactic nuclei, and accretion powered of the cold, solid-state local universe, by revealing a objects. Investigating photoionized plasma from afar rich mid-IR (M to N band) spectroscopy between 5 does not allow for many options when it comes to and 20 microns, associated with a wealth of icy mate- collecting data, nor does it allow for in depth system- rial in star-forming regions. Consequently an “aver- atic studies of changing plasma conditions. Study- age” interstellar ice “mix” has been proposed. Sub- ing laboratory photoionized plasmas afford greater sequently, AKARI observations have enabled us to control over the parameter space. Typically, labo- map the distributions of simple molecular ices, such ratory photoionized plasmas require large scale fa- as CO, CO2,H2O and CH3OH across star-forming cilities that are capable of producing a high inten- regions at unprescedented resolution — but these re- sity broadband x-ray flux. The use of supersonic gas sults strongly indicate small scale solid-state chem- jets as an interaction medium allows university scale ical varability — at least of scales down to ∼1000 pulsed power generators to perform laboratory pho- AU. And now ALMA is revealing a whole molecu- toionized plasma research. Supersonic gas jets can lar universe which (in the gas-phase at least) varies be placed much closer to an x-ray source and they on scales of only a few AU, and strongly hints that do not require any medium for containment or tamp- both chemical complexity and grain growth are fun- ing, thus avoiding x-ray flux attenuation. The exper- damentally dependent on ice contituents and prop- iments were carried out using the Zebra accelerator, erties. a 1 MA pulsed power generator, at the University of To fully understand what we are observing and Nevada Reno. Zebra is capable of producing 12-16kJ the role ices play in evolving the by-products of star- of x-ray energy, with photons under 1keV in energy, formation is a challenge that can only be resolved in from the implosion of z-pinch wire-arrays. Neon, ar- the laboratory. Three fundamental questions remain gon, and nitrogen gas has been investigated utiliz-

25 ing a variety of laser and x-ray diagnostics. Mach- There is a substantial effort in the physics commu- Zehnder interferometry, at 266nm, is used to char- nity to search for dark matter interactions with the acterize the neutral gas jet before the Zebra shot. of . The cosmic mi- Dual-color air-wedge interferometry, at 532nm and crowave background anisotropies are sensitive to en- 266nm, probe the electron density of the photoion- ergy injection from dark matter annihilations and to ized gas jet. Multi-color shadowgraphy, at 1064, 532, energy and momentum transfer due to dark matter and 266nm, is used for further characterization of the scattering with baryons. These effects enable a broad plasma. A cylindrically bent KAP crystal spectrom- search for dark matter interactions using cosmologi- eter measures the x-ray absorption spectrum. Inter- cal observations in a parameter space that is comple- ferometry and x-ray absorption spectroscopy show mentary to that of indirect and direct detection ex- electron areal densities of 1-3.5x1018 cm−2. Interfer- periments. In this talk, I will describe the effects of ometry measures electron densities in the range of 1- annihilation and scattering in cosmology and show 4x1019 cm−3. This work was sponsored in part by the constraints using Planck 2015 data. I will also discuss DOE NNSA HEDLP Grant DE-NA0003875, DOE Of- the implications of dark matter interactions during fice of Science Grant DE-SC0014451, and the ZFun- the era of Cosmic . damental Science Program. 115.04 — Searching for Dark Matter at Cosmic 115 — Cosmological Probes of Dawn Dark Matter I Julian B. Munoz1; Yacine Ali-Haimoud2; Abraham Loeb1; Cora Dvorkin1; Ely Kovetz3 1 Physics, Harvard University (Cambridge, Massachusetts, United 115.01 — Introductory comments States) Yacine Ali-Haimoud1 2 NYU (New York, New York, United States) 3 1 New York University (New York City, New York, United States) Ben Gurion (Beersheba, Israel)

I will make brief intrductory remarks for this special The nature of the dark matter is still a mystery, al- session on cosmological probes of dark matter. though current and upcoming 21-cm measurements during the cosmic dawn can provide a new arena on 115.02 — Dark matter interactions: CMB spectral the search for the cosmological dark matter. This era distortions and Neff. saw the formation of the first stars, which coupled the spin temperature of hydrogen to its kinetic tem- Yvonne Wong1 perature — producing 21-cm absorption in the CMB. 1 The University of New South Wales (Sydney, New South Wales, The strength of this absorption acts as a thermostat, Australia) showing us if the baryons have been cooled down or heated up by different processes. I will show what It is well known that elastic scattering between dark the 21-cm line can teach us about dark matter, focus- matter and a radiation component can lead to in- ing on the case of ”millicharged” dark-matter, which teresting phenomenologies on small-length scales, can explain the anomalous 21-cm depth observed by some of which can be exploited to alleviate, e.g., the the EDGES collaboration. so-called small-scale crisis of dark matter. In this talk I discuss some other phenomenlogies of this sce- 115.05 — Soft Spectral Distortions from Dark nario. In particular, I’ll explain how such an inter- Photons ation can also lead to signatures in the CMB energy spectrum in the form of spectral distortions, and how Joshua Ruderman1 elastic scattering can lead to a small change in the so- 1 Physics, New York University (New York, New York, United called effective of number of parameter. States)

115.03 — Studying Dark Matter Interactions with The Rayleigh-Jeans tail of the CMB is poorly con- the CMB strained at low energies, and therefore could be highly distorted from a blackbody consistent with Kimberly K. Boddy1 current measurements. I will describe how dark ra- 1 Johns Hopkins University (Baltimore, Maryland, United States) diation, composed of dark photons, can inject soft photons from resonant oscillations during the dark ages. A small fraction of the Universe’s energy in

26 dark photons can produce large distortions in the in a Bayesian framework to arrive at posterior dis- Rayleigh-Jeans tail. Measurements of cosmological tributions of parameters of interest given the avail- 21cm absorption test the CMB spectrum at low ener- able data. We perform Bayesian model comparison gies, because injected 21cm photons produce deeper of nested SED models by estimating the Bayesian absorption than the standard cosmology, as tenta- evidence. Our analysis is one of the first to make tively observed by the EDGES experiment. A smok- systematic use of the Bayesian model comparison ing gun of dark photon oscillations is the presence method to answer questions about galaxies’ star for- of sharp edges, as a function of redshift, in the 21cm mation histories and dust attenuation laws. Nested signal. sampling is superior to MCMC in this case becase it is suitable for handling multimodality of posteri- ors and non-normal likelihoods, parameter degen- 116 — Instrumentation: Ground eracies, and calculating the Bayesian evidence to an Based, Computation, etc. accurate level for model comparison. We use multi-wavelength photometric data from 116.01 — XL-Calibur: Plans for a Next-Generation the 3D-HST catalogs to model the spectral energy Hard X-ray Polarimeter distribution of galaxies at z=1, z=2, and z=3 in 23 bands. Kernel density estimation of both the obser- Quincy Abarr1 vational measurement errors and parameter space is 1 Physics, Washington University in St. Louis (St. Louis, Missouri, used in a tau model to generate realistic galaxy spec- United States) tra. We then fit the model parameters to this simu- lated data using nested sampling to verify the viabil- X-Calibur is a hard X-ray scattering polarimeter ity of both the model and the sampling algorithm. which flew for a short stratospheric balloon flight Another important byproduct of our analysis is from McMurdo, Antarctica during the 2018-2019 the direct testing of an analytic approximation of the austral summer. This flight resulted in preliminary Bayes factor, known as Savage-Dickey Density Ra- limits on the polarization properties of GX 301-2, an tio (SDDR), which is valid in the regime in which accreting pulsar. nested models are compared. We test this assump- Following up on this promising first result, here tion directly by comparing the Bayes factors ob- we will present plans for a successor mission: XL- tained through nested sampling and those obtained Calibur. This is based on the X-Calibur design, through the SDDR. but is expected to have sensitivity roughly six times We then assess the effects of software-specific greater. Upgrades include: thinner CZT detectors nested sampling implementations in SED fitting, in the polarimeter to reduce background; using the such as consistency of point estimates, how the num- spare mirror from the Hitomi satellite, which in- ber of the number of live points used in the nested creases the effective area in the key energy range of sampling run affect the efficiency and bias, and the 20-40 keV by four; and modified shielding around effect of dimensionality. Nested sampling runs can the polarimeter to further reduce background. be divided into independent ”threads”, which en- Using this upgraded instrument in two north- ables us to use standard resampling techniques such ern and one southern hemisphere balloon flights (in as bootstrapping to the set of threads to approxi- 2021, 2022, and 2024, respectively), we will be able to mate the entire error distribution without making as- observe both neutron stars, like GX 301-2, and black sumptions about its form. holes, like Cyg X-1. Polarimetric observations will provide systematically new information on the ge- 116.03 — Multi-component Decomposition of ometry of these sources and their surroundings. Astronomical Spectra by Compressed Sensing

116.02 — Bayesian Methods in Spectral Energy Mark Cheung1,2; Bart De Pontieu1,8; Juan Martinez- Distribution Fitting of Galaxies Sykora1; Paola Testa3; Amy R. Winebarger4; Adrian N. Daw5; Viggo Hansteen6,8; Patrick Antolin7; Theodore D. 1,2 2 Andrew Lawler ; Viviana Acquaviva Tarbell1; Jean-Pierre Wuelser1; Peter R. Young5 1 Baylor University (Waco, Texas, United States) 1 Lockheed Martin Solar & Astrophysics Lab (Palo Alto, California, 2 CUNY City Tech (Brooklyn, New York, United States) United States) 2 Stanford University (Stanford, California, United States) Bayesian statistical methods have been used in recent 3 Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- years to aid in SED fitting. Typically, Markov Chain sachusetts, United States) Monte Carlo sampling techniques have been used

27 4 NASA Marshall Space Flight Center (Huntsville, Alabama, Furthermore, much of the data from Pan-STARRS- United States) 1 was collected in surveys designed to meet a number 5 NASA Goddard Space Flight Center (Greenbelt, Maryland, of science objectives without being optimized for any United States) one of them. As a result, the discovery of moving ob- 6 University of Oslo (Oslo, Norway) jects in much of the data requires exposures collected 7 University of St Andrews (St Andrews, United Kingdom) over weeks, months, and years. Properly identifying 8 Rosseland Centre for Solar Physics (Oslo, Norway) and correcting the biases introduced by the sensitiv- ity irregularities of GPC1 used in such survey modes The signal measured by an astronomical spectrome- requires a more detailed survey simulator. ter may be due to radiation from a multi-component We present a survey simulator for Pan-STARRS-1 mixture of plasmas with a range of physical proper- that captures the relevant details of the detection of ties (e.g. temperature, Doppler velocity). Confusion moving objects, and we report the results of apply- between multiple components may be exacerbated ing this novel tool to our ongoing outer solar system if the spectrometer sensor is illuminated by overlap- searches. ping spectra dispersed from different slits, with each slit being exposed to radiation from a different por- tion of an extended astrophysical object. We use a 117 — Solar Physics Division compressed sensing method to robustly retrieve the Meeting (SPD), Corona 1 different components. This method can be adopted for a variety of spectrometer configurations, includ- 117.01 — Hi-C2.1 Observations of Solar Jetlets at ing single-slit, multi-slit (e.g., the proposed MUlti- Sites of Flux Cancelation slit Solar Explorer mission; MUSE) and slot spec- trometers (which produce overlappograms). Navdeep Panesar1; Alphonse C. Sterling1; Ronald L. Moore1 116.04 — An Efficient, High-Fidelity Survey 1 MSFC (Huntsville, Alabama, United States) Simulator for Pan-STARRS-1 Solar jets of all sizes are magnetically channeled Matthew J. Holman1; Matthew J. Payne1 narrow eruptive events; the larger ones are often 1 Harvard-Smithsonian, CfA (Cambridge, Massachusetts, United observed in the solar corona in EUV and coro- States) nal X-ray images. Recent observations show that the buildup and triggering of the minifilament Survey simulators are an essential tool for determin- eruptions that drive coronal jets result from mag- ing the efficiency and detection biases of searches for netic flux cancelation under the minifilament, at solar system bodies, as well as for developing and the neutral line between merging majority-polarity testing the algorithms. Without such tools, it is diffi- and minority-polarity magnetic flux patches. Here cult to determine the intrinsic populations underly- we investigate the magnetic setting of six on- ing the subset of objects observed. Such simulators disk small-scale jet-like/-like eruptions (also have been developed for CFEPS/OSSOS, NEOWISE, known as jetlets) by using high resolution 172A and other surveys, leading to detailed results on the images from the High-resolution Coronal Imager small body populations throughout the solar system. (Hi-C2.1) and EUV images from Solar Dynamics For those surveys, the detection of moving objects Observatory (SDO)/Atmospheric Imaging Assem- results from the analysis of a small number of ex- bly (AIA) and line-of-sight magnetograms from posures taken over a relatively short period of time. SDO/Helioseismic and Magnetic Imager (HMI). Therefore, the survey simulators focus on the num- From magnetograms co-aligned with the Hi-C and ber of objects that appear in each field of view within AIA images, we find that (i) these jetlets are rooted the survey, as well as the magnitudes of those ob- at edges of magnetic network lanes (ii) some jetlets jects. stem from sites of flux cancelation between merging Giga-Pixel Camera-1 (GPC1) on the Pan-STARRS-1 majority-polarity and minority-polarity flux patches telescope has a large, 3 degree diameter field of view, (iii) some jetlets show faint brightenings at their with a focal plane tiled with 60 detectors, each of bases reminiscent of the base brightenings in coronal which contains 64 independently-addressable cells. jets. Based on the 6 Hi-C jetlets that we have exam- There are physical gaps between the detectors and ined in detail and our previous observations of ∼30 insensitive regions between the cells. In addition, coronal jets in quiet regions and coronal holes, we in- many of the cells are either dead or noisy. fer that flux cancelation is the essential process inthe

28 buildup and triggering of jetlets. Our observations sheared/twisted core field or flux rope along and suggest that network jetlets result from small-scale above the cancellation line) to explode. In types eruptions that are analogs of both larger-scale coro- I & II the explosion is confined, while in type III nal jet minifilament eruptions and the still-larger- the explosion is ejective and drives jet-like outflow scale eruptions that make major CMEs. This work in the manner of larger jets in coronal holes, quiet was supported by the NASA/MSFC NPP program regions, and active regions. and the NASA HGI Program. 117.03 — The life of coronal bright points

117.02 — Fine-scale explosive energy release at 1 2 sites of magnetic flux cancellation in the core of Karin Muglach ; Andrew Leisner 1 GSFC (Greenbelt, Maryland, United States) the solar active region observed by HiC2.1, IRIS 2 and SDO UMD (College Park, Maryland, United States) Sanjiv K. Tiwari1; Navdeep Panesar2; Ronald L. Moore2; Coronal bright points are small-scale magnetic re- Bart De Pontieu3; Paola Testa4; Amy R. Winebarger2 gions found all over the solar disk. They are visi- 1 LMSAL/BAERI (Palo Alto, California, United States) ble in coronal emission lines which sample plasma 2 NASA/MSFC (Huntsville, Alabama, United States) at around 1-2 MK. In this study we follow the com- 3 LMSAL (Palo Alto, California, United States) plete lifetime of several coronal bright points, from 4 SAO (Cambridge, Massachusetts, United States) the time they appear in the SDO/AIA coronal filter- grams to the time they fade again into the quiet solar The second sounding-rocket flight of the High- background emission. In addition to the hot coro- Resolution Coronal Imager (HiC2.1) provided nal emission, lower temperature chromospheric fil- unprecedentedly-high spatial and temporal reso- tergrams (e.g. AIA 304 Å) sometimes show the for- lution (150 km, 4.5 s) coronal EUV images of Fe mation of dark absorption structures similar to fil- IX/X emission at 172 Å, of a solar active region aments. From SDO/HMI we can get the accompa- (AR NOAA 12712) near solar disk center. Three nying evolution of the photospheric magnetic flux morphologically-different types (I: dot-like, II: density and also calculate the plane-of-sky plasma loop-like, & III: surge/jet-like) of fine-scale sud- flow field using local correlation tracking. Mostof den brightening events (tiny microflares) are seen the coronal bright points show some jet activity dur- within and at the ends of an arch filament sys- ing their lifetime and these data allow to us to study tem in the core of the AR. We complement the both the energy buildup of the coronal bright point 5-minute-duration HiC2.1 data with SDO/HMI and the initiation of the jets. magnetograms, SDO/AIA EUV and UV images, and IRIS UV spectra and slit-jaw images to examine, 117.04 — Polarimetric observations of the SiX and at the sites of these events, brightenings and flows Fe XIII infrared coronal emission lines using the in the transition region and corona and evolution of SOLARC telescope magnetic flux in the photosphere. Most, if not all, 1 2 of the events are seated at sites of opposite-polarity Gabriel Dima ; Jeffrey Richard Kuhn ; Thomas A. 1 magnetic flux convergence (sometimes driven by Schad 1 adjacent flux emergence), implying flux cancellation National Solar Observatory (Makawao, Hawaii, United States) 2 at the polarity inversion line. In the IRIS spectra and Institute for Astronomy, University of Hawaii (Makawao, Hawaii, images, we find confirming evidence of field-aligned United States) outflow from brightenings at the ends of loops of The forbidden Si X emission line at 14301 Å has been the arch filament system. These outflows from identified as a potentially valuable polarized diag- both ends of the arch filament system are seen as nostic for solar coronal magnetic fields; however, the bi-directional flows in the arch filament system, only polarized Si X measurements achieved to date suggesting that the well-known counter-streaming have been during eclipses and at comparatively low flows in large classical filaments could be drivenin spatial and spectral resolution. Here we report spec- the same way as in this arch filament system: by tropolarimetric observations of both the Si X 14301 fine-scale jet-like explosions from fine-scale sites of mixed-polarity field in the feet of the sheared Å and more well-established FeXIII 10747 Å coro- field that threads the filament. Plausibly, the flux nal lines acquired with the 0.45 m aperture SOLARC cancellation at these sites prepares and triggers coronagraph atop Haleakala. Results for both lines, a fine scale core-magnetic-field structure (a small which represent averages over different active and non-active regions of the corona, indicate a relatively

29 flat radial variation for the line widths and line cen- an individual loop’s field strength and twist. Ul- ters and a factor of ∼2-3 decrease in polarized bright- timately, we find the rate of newly-brightened flux ness between 1.05 and 1.45 R⊙. Averaging over all overestimates the flux which could be undergoing the measurements the mean and standard deviations reconnection. This excess can be explained by our of line properties for Si X 14301 Å and Fe XIII 10747 finding that the interconnecting region is not atits Å are respectively: FWHM of 3.0±0.4 Å and 1.6±0.1, lowest energy (constant-α) state; the LFFF model- line-integrated polarized brightness of 0.07±0.03 and ing shows a variation in values of α. This overesti- 0.3±0.3 erg s−2 cm−2 sr−1 where the uncertainty mate might be the result of the region’s unusually quoted reflects a large sample variance, and line cen- slow emergence, providing time for internal Taylor- ter wavelengths 14300.7±0.2 Å and 10746.3±0.1 Å. relaxation reconnection of the interconnecting flux The polarized brightness for both lines may be un- following its initial formation by reconnection. We derestimated by up to a factor of 5 due to limitations support this hypothesis by computing the rates of in the photometric calibration. When accounting for brightening within the plane of the virtual slit. This this uncertainty we find consistency between our ob- work was supported by NASA’s HGI program. servations and previous measurements of the two lines as well as theoretical calculations and affirm the 117.06 — Constraints from Hinode/EIS on the potential of the Si X line as a polarized diagnostic of Expansion of Active Region Loops Along the Line the solar corona. of Sight Therese A. Kucera1; Peter R. Young1; James A. 117.05 — Measuring and modeling the rate of Klimchuk1; Craig DeForest2 separator reconnection between an emerging and 1 NASA GSFC (Greenbelt, Maryland, United States) existing active region 2 Southwest Research Institute (Boulder, Colorado, United States) Marika McCarthy1; Dana Longcope1; Anna Malanushenko2; David Eugene McKenzie3 We explore the constraints that can be placed on 1 Montana State University (Bozeman, Montana, United States) the dimensions of coronal loops out of the plane of 2 HAO (Boulder, Colorado, United States) the sky by utilizing spectroscopic observations from 3 MSFC (Huntsville, Alabama, United States) the Hinode/EUV Imaging Spectrometer (EIS). The usual assumption is that loop cross sections are cir- Magnetic reconnection must occur when new flux cular. Changes in intensity not constant with the emerges into the corona and becomes incorporated measured width are assumed to be the result of into the existing coronal field. A new active region changing density and/or filling factor. Here we (AR) emerging in the vicinity of an existing AR pro- instead focus on the possibility that the loop di- vides a convenient laboratory in which reconnection mensions may be changing along the line of sight of this kind can be quantified. We perform such a while the filling factor remains constant. We ap- measurement using high time-cadence 171 Å data ply these ideas to two cool (5.5

30 118 — Solar Physics Division course of their lifetimes. Here we will discuss the work being done to validate and advance the AFT Meeting (SPD), Data & model. We will discuss the ability of AFT to repro- Computation duce other active region properties, such as tilt an- gles, polarity separation, area expansion and mag- 118.01 — Fractal Dimensions of Solar and netic elements size distribution, for simple and more Geomagnetic Indices complex active regions. Currently, AFT uses data assimilation to incorporate the magnetic field from W. Dean Pesnell1 magnetograms from the Earth’s vantage point. We 1 NASA GSFC (Greenbelt, Maryland, United States) will also discuss the work that is being done to de- velop an automated process for adding in far-side ac- Correlations between solar and geomagnetic indices tive regions observed by STEREO in 304 Å. are often used in space weather research. How sen- sitive are these correlations to pre-whitening of the 118.03 — Mapping the Sun’s Far-Side Magnetic data and auto-correlation within the data sets? Sta- Flux through a Machine-Learning Code Trained tistical and timeseries analyses of the sunspot num- by Use of the Sun’s Near-Side Observations ber are often used to predict solar activity. These methods have not been completely successful as the Ruizhu Chen1; Junwei Zhao1 changes over time and one cycle’s 1 Stanford University (Stanford, California, United States) sunspots are not a faithful predictor of the next cy- cle’s activity. Can more accurate predictions be pro- The Sun’s far-side magnetic field is crucial to space duced by partitioning the data into periods when it weather forecasting and solar wind modeling, but it obeys certain statistical properties? The Hurst expo- cannot be directly observed. For about four years, nent and the related fractal dimension are two such the extreme ultraviolet (EUV) 304Å flux of the far ways to partition the data. We can use these mea- side was observed by the STEREO/EUVI, provid- sures of complexity to compare the sunspot number ing a chance for us to map the far-side magnetic flux with other solar and geomagnetic indices. We use using a machine-learning method. We take about five algorithms to calculate the Hurst exponent or 6000 near-side SDO/HMI magnetic-field maps and fractal dimension and examine what happens when SDO/AIA 304Å flux images, observed simultane- the mean and a linear trend trends are removed. ously and covering a period of about 8 years, and We find that some algorithms are robust and return train a neural-network that is able to convert the EUV similar or identical values for the original, mean- flux images into magnetic-flux maps. The trained removed, and linear-trend-subtracted data. The be- network is then applied on a test set of SDO/AIA havior of the Fourier transform at low frequencies is data, and the results are then compared with the the most sensitive to the type of pre-whitening ap- SDO/HMI magnetic-field observations. Satisfactory plied to the data. The rescaled-range algorithm is ro- agreements are found between the observations and bust but needs to be corrected for autocorrelation in the computer-generated maps. The trained machine- the data. learning code is then applied on the STEREO far- side 304Å observations to generate the far-side mag- 118.02 — Advancing the Advective Flux Transport netic flux maps. These data are useful to assess the Model validity of the far-side magnetic field produced by flux-transport models, and to examine the solar wind Lisa Upton1; Ignacio Ugarte-Urra2; Harry Warren2 1 models with and without including the far-side mag- Space Systems Research Corportation (Alexandria, Virginia, netic field. United States) 2 Naval Research Laboratory (Washington, District of Columbia, 118.04 — New Space Weather Climate Record of United States) the Solar Spectral Irradiance Variability over Solar The Advective Flux Transport (AFT) model has Cycles 23 and 24 proven to be a reliable surface flux transport model Thomas N. Woods1; Francis Eparvier1 for describing the evolution of the global magnetic 1 Univ. of Colorado (Boulder, Colorado, United States) field, accurately reproducing the evolution of the po- lar field. AFT has also been shown to accurately The solar irradiance is the primary natural energy (within a factor of 2) reproduce the evolution of the input into Earth’s atmosphere and climate system. total unsigned flux of simple active regions over the Understanding the long-term variations of the solar

31 spectral irradiance (SSI) over time scales of the 11- this data gap. The calibration will employ machine- year solar activity cycle and longer is critical for most learning methods that use EUV 304 Å data as a Sun-climate research topics. Of particular interest for bridge: a relation will be sought 1) between the near- the space weather community is the long-term varia- side AIA 304 Å data and HMI magnetic field data, tions of the solar extreme ultraviolet (EUV: 100-1250 and 2) between STEREO 304 Å data and far-side he- Å) and soft X-ray (SXR: 10-100 Å) because those en- lioseismic images obtained from a newly developed ergetic photons create Earth’s ionosphere and heat time-distance helioseismic far-side imaging method. Earth’s thermosphere. Consequently, the solar EUV As an update, progress has been made in establish- and SXR variability is important for several space ing the relation between the near-side 304 Å data and weather studies, such as understanding changes in magnetic flux data, and some previously-unknown the thermospheric density that affect satellite drag systematics were identified and corrected in the he- (and thus satellite life times). lioseismic far-side images. These systematic-effect- There are on-going daily satellite measurements corrected far-side images will then be used to estab- of the EUV and SXR SSI since 2002. These are be- lish a relation with the far-side EUV data. ing combined to create a new space weather climate record for the SSI in the 5 to 1900 Å range to un- 118.06 — HelioML: An interactive online book at derstand the long-term variability over Solar Cycles the crossroads of heliophysics and machine 23 and 24. The primary SSI observations are from learning containing the code behind published the Solar Dynamics Observatory (SDO) EUV Vari- papers ability Experiment (EVE) and Thermosphere, Iono- sphere, Mesosphere, Energetic, Dynamics (TIMED) James Paul Mason1; Monica Bobra2 Solar EUV Experiment (SEE). A limiting factor for 1 Solar Physics Laboratory, NASA Goddard Space Flight Center the accuracy in making a composite SSI record is (Greenbelt, Maryland, United States) the uncertainty in the various instrument degrada- 2 Stanford University (Stanford, California, United States) tion corrections. A new analysis technique for trend- ing SSI time series is helping to identify some un- The subcomponents of artificial intelligence, ma- corrected instrumental trends, which, once applied chine and deep learning, have already been used in to the SSI trends, can improve the long-term SSI ac- peer-reviewed papers in heliophysics. In order to curacy. The SDO and TIMED time series, this new understand these papers as readers and as peer re- technique for trending, and the new composite SSI viewers, we need to have at least a passing familiarity record will be presented. with how these new techniques work. It’s not magic but it’s not trivial either. We set out to make an on- 118.05 — Reliably Inferring the Sun’s Far-Side line book with code examples and lots of explanatory Magnetic Flux for Operations Using text to show how machine/deep learning have actu- Time-Distance Helioseismic Imaging - Updates ally been employed in heliophysics research to date. Everything in the book is written in open source Shea A. Hess Webber1; Junwei Zhao1; Ruizhu Chen1; python. There’s an “Interact” button at the top of Jon Todd Hoeksema1; Yang Liu1; Monica Bobra1; Marc each chapter that, with one click, will spin up a com- L. DeRosa2 puter in the cloud for you and 10 seconds later you 1 HEPL, Dept. of Physics, Stanford University (Stanford, Califor- can edit and execute the code in the chapter. Or you nia, United States) can download the code and play with it locally. Each 2 Lockheed Martin (Palo Alto, California, United States) chapter is written by a contributor and is associated with a published paper. We’re also looking for more. Solar wind models are highly dependent on global We presently cover a variety of heliophysics and ma- magnetic fields at the solar surface as their inner chine learning topics (see full list here [1]): Classi- boundary condition, and the lack of global field data fication, model selection, image processing, regres- is a significant problem plaguing solar wind model- sion, image transformation; space weather predic- ing. Currently, only near-side magnetic field obser- tion from magnetograms, image resolution enhance- vations exist and far-side approximations are inca- ment, and simulating data from a lost instrument. pable of predicting growth of existing active regions Check the book out here [2] and the source code is or new magnetic flux emergence. We therefore plan here [3]. to develop a method that calibrates far-side helio- [1] https://helioml.github.io/HelioML/01/2/ seismic images, calculated using near-side Doppler in_this_book [2] http://helioml.org [3] https:// observations, to far-side magnetic flux maps to fill github.com/HelioML/HelioML

32 119 — Helen B. Warner Prize we have discovered a breath taking array of extraso- lar planets (or exoplanets). Understanding the atmo- Lecture: Hunting for Dark Matter spheres and underlying surfaces of these planets is of in the Early Universe, Yacine tremendous interest, but the presence of clouds and hazes pose great challenges for direct observation of Ali-Haïmoud (New York these features. University) Despite the challenge I hope to convince you that we don’t need to see through the clouds to learn about 119.01 — Hunting for dark matter in the early the underlying atmosphere, but rather we can use Universe the physical properties of exoplanet cloud particles to our advantage. One way to do this is through careful, Yacine Ali-Haimoud1 laboratory-based measurements of scattering and 1 New York University (New York, New York, United States) the polarization of scattered light by exoplanet cloud analogs. It is now well established that a large part of the mat- The physical properties of cloud particles (size, ter in the Universe is some substance which appears shape, composition) and how they interact with light to be oblivious to any force but gravity. The nature are explicitly tied to their trajectory through, or his- of this “dark matter” remains a mystery. Could it tory within, an atmosphere. Thus, the thermody- be a new particle, as light as an electron, or might namic conditions, atmospheric chemistry, dynami- it be made of black holes as massive as many ? cal processes, and nucleation mechanisms to which In this talk, I will first describe how one can hope to the particle was exposed all play a role in determin- tease out some of the properties of dark matter from ing its physical properties and the way it scatters the Cosmic Microwave Background (CMB), the relic and polarizes light. We will discuss how laboratory- radiation from the very early Universe. I will review based measurements of scattering and polarization the basic physics underlying the CMB, in particular are currently being conducted, how this data can why it has a nearly perfect blackbody spectrum, and start to pin down signals in light scattered by exo- what the tiny changes of temperature across the sky planet clouds, and how it might be used to identify tell us about the history and contents of the Universe. cloud properties from planetary phase curves in the I will then illustrate how precise measurements of future. We will also discuss what this data can teach the CMB properties may inform us about the na- us about portions of an atmosphere we cannot ob- ture of dark matter. Last but not least, I will explain serve, such as below an optically thick cloud deck, how gravitational waves, recently directly detected and improve our understanding of radiative balance by LIGO, may provide an entirely new window into in these exotic systems. the mystery of dark matter. 121.02 — Laboratory Exploration of 121 — Laboratory Astrophysics Photochemistry and Aerosol Formation in Exoplanet Atmospheres Division Meeting (LAD): Bridging Nikole K. Lewis1 Laboratory and Astrophysics: 1 Cornell University (Baltimore, Maryland, United States) Exoplanets I The importance of photochemistry and aerosols (clouds and hazes) in the atmospheres of solar sys- 121.01 — Exploring Exoplanet Clouds at Home tem objects has long been recognized. As observa- and Abroad tions aimed at characterizing the atmospheres of ex- Alexandria V. Johnson1 oplanets have increased in fidelity, it has become 1 Earth, Environmental and Planetary Sci, Brown University clear that aerosols and photochemistry also play (Providence, Rhode Island, United States) a critical role in planets beyond our solar system. The phase space of stellar irradiation, temperature, From the shrouds of and to Jupiter’s chemical composition, and planetary size spanned great red spot and the veil of Pluto, clouds and by exoplanets is much greater than that spanned by hazes are a ubiquitous feature of the planetary atmo- planets in the solar system, which limits our ability spheres in our solar system. As we extend our gaze to leverage solar system analogs to understand key beyond to learn about our nearest stellar neighbors atmospheric processes. Recently, efforts have begun to explore photochemistry and aerosol formation in

33 exoplanet atmospheres through laboratory simula- that allows the simulation of Titan’s complex atmo- tions of the relevant environments. In this talk, I spheric chemistry at Titan-like temperature (200 K). will provide an overview of results from laboratory We will also introduce a new study of the optical explorations of exoplanet atmospheres and discuss properties of ammonium-bearing phosphates, po- future needs. With a new wave of exoplanet obser- tential cloud particles forming in temperate exoplan- vations coming in the next decade from ground and ets and brown dwarfs. space-based facilities, such as JWST, laboratory work Acknowledgements: The authors acknowledge focused on exoplanet photochemistry and aerosol the technical support of Emmett Quigley. formation will prove increasingly critical for under- standing these distant worlds. 121.04 — Dust Evolution in the Late Stages of Planet Forming Disks 121.03 — The new NASA Ames Infrared Optical This is an additional presentation of abstract 105.06. See Constant Facility. Determinations for Titan that entry for details. Aerosol-, and Exoplanet and Cloud Particle Analogs Ella Sciamma-O’Brien1; Ted L. Roush1; David F. 122 — Stars & Stellar Topics I Dubois1,2; Caroline Morley3; Mark S. Marley1; Farid Salama1 122.01 — Effective of Low-Mass 1 NASA Ames Research Center (Moffett Field, California, United Stars from High-Resolution H-band Spectroscopy States) 1 1 2 Ricardo Lopez-Valdivia ; Gregory N. Mace ; Kimberly Bay Area Environmental Research Institute (Moffett Field, Cali- R. Sokal1; Daniel Thomas Jaffe1 fornia, United States) 1 Astronomy, The University of Texas at Austin (Austin, Texas, 3 University of Texas at Austin (Austin, Texas, United States) United States)

Here we present a new optical constant facility de- High-resolution, near-infrared spectra will be the veloped at NASA Ames that will allow the deter- primary tool for finding and characterizing Earth- mination of optical constants in the infrared of var- like planets around low-mass stars. Yet, the prop- ious materials, analogs of hazes and cloud parti- erties of exoplanets can not be precisely determined cles in (exo)planet atmospheres and brown dwarfs. without accurate and precise measurements of the Our facility is composed of a Fourier Transform In- host star. Spectra obtained with the Immersion frared (FTIR) spectrometer continuously covering GRating INfrared Spectrometer (IGRINS) simultane- the Near-IR, mid-IR and Far-IR range (from 0.74 ously provide diagnostics for most stellar parame- to 200 µm), coupled to variable angle transmit- ters, but the first step in any analysis is the determi- tance and reflectance accessories that allow the char- nation of the . Here we report acterization of the scattering properties of nonho- the calibration of high-resolution H-band spectra to mogeneous samples (laboratory planetary aerosol accurately determine effective temperature for stars analogs, films, slabs of material, crystals, powders…) between 4000-3000 K (∼K8 – M5) using absorption over a wide incidence and emittance angle range line depths of Fe, OH, and Al. The field star sample (0-90 degrees). This permits the angular light dis- used here contains 254 K and M stars with temper- tribution in both transmission and reflection mea- atures derived using BT-Settl synthetic spectra. We surements to be characterized, enabling the deter- use 106 stars with precise temperatures in the liter- mination of the complex indices of refraction, n and ature to calibrate our method with typical errors of k, over the full NIR-FIR range via modeling of the about 140 K, and systematic uncertainties less than laboratory observations. The resulting refractive in- ∼120 K. For the broadest applicability, we present dices are critical input parameters in radiative trans- Teff – line-depth-ratio relationships, which we test on fer models, exoplanet and brown dwarf cloud mod- 12 members of the TW Hydrae Association and at els, protoplanetary disk simulations and other mod- spectral resolving powers between ∼10,000–120,000. els used for the interpretation of observational data These ratios offer a simple but accurate measure of from past, current and future (exo)planetary NASA effective temperature in cool stars that is distance missions. We will present preliminary data obtained and reddening independent. on Titan aerosol analogs produced in the Titan Haze Simulation (THS) experiment on COSmIC, a unique experimental platform developed at NASA Ames

34 122.02 — Do Kepler superflare stars really include for superflares, considering long-term (1,000-10,000 slowly-rotating Sun-like stars ? - Results using years) activity level changes. APO 3.5m telescope spectroscopic observations and Gaia-DR2 data - 122.03 — Probing the Origins of Intense Magnetism in Early M-Dwarf Stars Yuta Notsu1,2; Hiroyuki Maehara3; Satoshi Honda4; Suzanne L. Hawley5; James R. A. Davenport5; Ko- Connor Bice1; Juri Toomre1 1 1,6 1 suke Namekata ; Shota Notsu ; Kai Ikuta ; Daisaku 1 Astrophysical and Planetary Sciences, University of Colorado at 1 1 Nogami ; Kazunari Shibata Boulder (Boulder, Colorado, United States) 1 Department of Astronomy, Kyoto University (Kyoto, Japan) 2 University of Colorado Boulder (Boulder, Colorado, United States) M-type stars are quickly stepping into the forefront 3 Okayama Branch Office, NAOJ (Asakuchi, Japan) as some of the best candidates in searches for habit- 4 University of Hyogo (Sayo, Japan) able Earth-like exoplanets, and yet many M-dwarfs 5 University of Washington (Seattle, Washington, United States) exhibit extraordinary flaring events which would 6 Leiden University (Leiden, Netherlands) bombard otherwise habitable planets with ionizing radiation. In recent years, observers have found Solar and stellar flares are the energetic explosions that the fraction of M-stars demonstrating significant in the solar and , and superflares magnetic activity transitions sharply from roughly 4 are very large flares that release total energy 10∼10 10% for main-sequence stars earlier (more massive) times greater than that of the biggest solar flares than spectral type M3.5 (0.35 M ) to nearly 90% for 32 ⊙ (∼10 erg). Recent Kepler-space-telescope observa- stars later than M3.5. Stellar dynamos are are driven tions found more than 1000 superflares on a few hun- primarily by fluid motions in the , dred solar-type stars. We report the latest view of the base of which migrates inward with decreasing Kepler solar-type (G-type main-sequence) superflare . Suggestively, it is also later than M3.5 stars, including recent updates with Apache Point at which main-sequence stars become fully convec- Observatory (APO) 3.5m telescope spectroscopic ob- tive, and may no longer contain a . This servations and Gaia-DR2 data. First, more than layer of rotational shear separating the convection half (43 stars) are confirmed to be “single” stars, and radiative zones is thought to play a significant among 64 superflare stars in total that have been role in solar magnetism, and so we here investigate spectroscopically investigated so far in this APO3.5m its influence on M-dwarf dynamos. Using the spher- and our previous Subaru/HDS observations. The ical 3D MHD simulation code Rayleigh, we compare measurements of v sin i (projected rotational veloc- the convective flows, magnetic field configurations ity) and chromospheric lines (Ca II H&K and Ca II and generation, and time dependencies of dynamos 8542 A) support the brightness variation of super- operating within quickly rotating M2 (0.4 M⊙) stars flare stars is caused by the rotation of a star with spanning a range of rotation rates and diffusivities, large . Then, we investigated again the sta- with the computational domain either terminating at tistical properties of Kepler solar- type superflare the base of the convection zone or permitting over- stars by incorporating Gaia-DR2 stellar radius val- shoot into the underlying stable region. We find that ues. As a result, the maximum superflare energy a tachocline is not necessary for the organization of continuously decreases as the Prot strong (10-20 kG) toroidal wreaths of magnetism in 34 increases. Superflares with their energy <∼ 5×10 these stars, though its presence can increase the cou- erg would occur on old slowly-rotating Sun-like stars pling of mean field amplitudes to the stellar rota- (Prot ∼25 days) once every 2000–3000 years, while tion rate and in some cases drastically alter the char- young rapidly- rotating stars with Prot ∼ a few days acter of the fields produced. Additionally, in stars 36 have superflares up to 10 erg. The maximum that undergo periodic magnetic cycles, we find that area does not depend on the rotation period the presence of a tachocline makes these cycles both when the star is young rapidly- rotating, but as the longer and more regular than they would have other- rotation slows down, it starts to steeply decrease at wise been. Finally, we find that the tachocline helps Prot ∼12 days for Sun-like stars. These two decreas- to enhance the surface poloidal fields and organize ing trends can be consistent since the magnetic en- them into larger spatial scales, both of which provide ergy stored around starspots explains the flare en- favorable conditions for more rapid angular momen- ergy, but other factors like spot magnetic structure tum loss through a magnetized stellar wind. should be also considered. These results presented in this work support that even slowly-rotating stars similar to the Sun can have large starspots necessary

35 122.04 — Double Trouble: Biases Caused by to the Sun. Models of stellar convection show too Binaries in Large Datasets sharp a transition to the interior adiabatic gradient, leading to a mismatch between computed and ob- Gregory Vahag Aghabekian Simonian1 1 served oscillation frequencies. We suggest that there Astronomy, The Ohio State University (Columbus, Ohio, United is a common solution to these problems: convec- States) tive motions in stellar envelopes are even more non- local than numerical models suggest. Small scale The volume of stellar rotation data has expanded photospherically driven motions dominate convec- greatly due to the advent of large-scale spectro- tive transport even at depth, descending through a scopic and high-precision photometric time-domain very nearly adiabatic interior (more nearly adiabatic surveys. However, the presence of binaries can in the mean than numerical models achieve). To test bias the interpretation of stellar rotation in these this, we develop a simple model that reproduces the datasets. I found that the rapid rotators in the Kepler mean thermodynamic stratification of three dimen- field are consistent with being a background tidally- sional hydrodynamic stellar envelope models. It can synchronized population, which would inflate the recover the mean thermodynmaic states of the full number of young stars interpreted through a single- models knowing only the filling factor and entropy star gyrochronology. By evaluating the quality of fluctuations of the granular downflows in their pho- APOGEE spectroscopic v sini in the Kepler field, tospheres. The supergranular scale of convection is I discovered that spectral blending of equal lumi- then determined by the depth to which the presence nosity binaries can mimic rotational broadening for of granular downflows alters the otherwise adiabati- velocity offsets near APOGEE’s spectral resolution. cally stratified background. The supergranular scale This effect can dominate over true rapid rotators for of convection is then determined by the depth to old stellar populations. However, for systems where which the presence of granular downflows alters the the of the secondary is negligible, I found otherwise adiabatically stratified background. that the APOGEE vsini are reliable. I will discuss strategies to improve the interpretations of rotation by either filtering likely binaries, or modeling their 122.06 — Nonlinearly damped oscillation modes effects. in red giants Nevin Weinberg2; Phil Arras1 122.05 — on the Sun and stars: 1 University of Virginia (Charlottesville, Virginia, United States) A simple model for its length scale 2 Massachusetts Institute of Technology (Cambridge, Mas- sachusetts, United States) Mark Rast1; Regner Trampedach2 1 University of Colorado (Boulder, Colorado, United States) 2 Turbulent motions in the convective envelope of red Space Science Institute (Boulder, Colorado, United States) giants excite a rich spectrum of solar-like oscillation modes. Observations by CoRoT and Kepler have Turbulent convection in stellar envelopes is critical shown that the mode amplitudes increase dramati- to heat transport and dynamo activity. Modeling it cally as the stars ascend the branch, i.e., as well it has proven surprisingly difficult, and recent the frequency of maximum power, ν , decreases. solar and stellar observations have raised questions max Most studies nonetheless assume that the modes are about our understanding of the dynamics of both well described by the linearized fluid equations. We the deep solar convection and the mean structure of investigate to what extent the linear approximation is the upper layers of convective stellar envelopes. In justified as a function of stellar mass Mandν , fo- particular, the amplitude of low wavenumber con- max cusing on dipole mixed modes with frequency near vective motions in both local area radiative magne- ν . A useful measure of a mode’s nonlinearity tohydrodynamic and global spherical shell magne- max is the product of its radial wavenumber and its ra- tohydrodynamic simulations of the Sun appear to dial displacement, k ξ (i.e., its shear). We show be too high. In global simulations this results in r r that k ξ ∝ ν −9/2, implying that the nonlinear- weaker than needed rotational constraint of the mo- r 푟 max ity of mixed modes increases significantly as a star tions and consequent non solar-like differential ro- evolves. The modes are weakly nonlinear (k ξ > tation profiles. In deep local area simulations it r r 10−3) for ν < 150 μHz and strongly nonlinear (k ξ yields strong horizontal flows in the photosphere on 푚푎푥 r r > 1) for ν < 30 μHz, with only a mild dependence scales much larger than the observed supergranu- max on M over the range we consider (1.0 - 2.0 M ). A lation, leaving the origin of the solar supergranu- ⊙ weakly nonlinear mixed mode can excite secondary lar scale enigmatic. The problems are not confined

36 waves in the stellar core through the parametric in- based on its rather variable intervals, the next erup- stability, resulting in enhanced, but partial, damp- tion should start in 2021±6. V394 CrA, CI Aql, V3890 ing of the mode. By contrast, a strongly nonlinear Sgr, and V2487 Oph should go off any year now, but mode breaks as it propagates through the core and is there is no high confidence for setting a date. fully damped there. Evaluating the impact of nonlin- ear effects on observables such as mode amplitudes and linewidths requires large mode network simu- 123 — Cosmological Probes of lations. We are currently carrying out such calcu- Dark Matter II lations and investigating whether nonlinear damp- ing can explain why some red giants exhibit dipole 123.01 — Placeholder: Celine Boehm modes with unusually small amplitudes, known as depressed modes. 123.02 — Early Structure Formation in LPBH Cosmologies 122.07 — Predictions for Upcoming Recurrent Derek Inman1; Yacine Ali-Haimoud1 Novae Eruptions; T CrB in 2023.6±1.0, U Sco in 1 New York University (New York, New York, United States) 2020.0±0.7, RS Oph in 2021±6, and more Primordial black holes (PBH) comprising some frac- Bradley E. Schaefer1 tion of the Universe’s dark matter is a potentially 1 Louisiana State Univ. (Baton Rouge, Louisiana, United States) interesting alternative to the more standard particle The prediction of upcoming recurrent erup- based dark matter. If the fraction is large, PBHs can tions has good utility for promoting a frequent significantly alter how and when nonlinear struc- watch so that the usually-very-short eruptions are tures develop. If it is small, they could provide po- not missed and caught early, plus allowing for the tentially interesting constraints on WIMPs and/or pre-organization of intense observing campaigns. seed the super massive black holes known to exist by Such efforts are highlighted by my prediction ofthe redshift ∼7. We have run LPBH cosmological simu- 2010 eruption of U Sco, where spacecraft targets-of- lations of structure formation starting from deep in opportunity programs were in place in advance and the radiation era and ending at z=100. We analyze workers watched the target several times a day for the clustering, structure and mass function of halos over a year, then resulting in measured magnitudes in the simulation, as well as typical PBH velocities averaging every three minutes for the entire erup- relevant for CMB constraints. Future use cases in- tion, plus daily and hourly spectra and UBVRIJHK clude tidal perturbations on primordial PBH binaries photometry, plus X-ray, gamma-ray, far-IR, IR, and and whether the formation of stars differs in this sce- UV spacecraft observations, leading to the all-time nario. best observed nova eruption and the discovery of two new phenomena. Recurrent novae are a particu- 123.03 — Probing the nature of dark matter with larly important subset of all novae, and they have the astrophysical and gravitational waves advantage that their eruptions can be predicted with observations useable accuracy. Inter-eruption times can be pre- 1 1 1 dicted from the brightness during quiescence, and Gianfranco Bertone ; Adam Coogan ; Daniele Gaggero 1 by looking at the history of inter-eruption intervals. University of Amsterdam (Amsterdam, Netherlands) For T CrB, with eruptions in 1866 and 1946, a sim- ple constancy of interval suggests the next eruption The formation and growth of black holes inevitably will be in 2026. But a better prediction is based on modifies the dark matter distribution around them. the pre-eruption-plateau with a rise to the plateau If dark matter is in the form of self-annihilating from 1936.0-1939.6 before the fast 1946.1 eruption, weakly interacting massive particles (WIMPs), the so with T CrB showing the same rise from 2014.2- increase in dark matter density can significantly 2016.4 up to the current plateau, the next eruption boost the annihilation rate. In the case of primor- will be in 2023.6±1.0. For the long history of intervals dial black holes (PBHs), a stringent constraints on for U Sco (averaging 10.6 years), the next eruption their cosmological abundance has been obtained by should come in 2020.7±1.6. But U Sco was substan- comparing the gamma-ray background produced by tially bright in 2011-2012, with higher accretion, so it WIMP annihilations around them with the one ob- should accumulate the trigger mass substantially be- served by Fermi-LAT. Here, we take the opposite fore 2020.7. Given that it has not erupted as of this viewpoint. We focus on the prospects for discov- writing, I predict a date of 2020.0±0.7. For RS Oph, ering PBHs with upcoming radio and gravitational

37 waves searches, and on the implications such a dis- within later-forming minihalos more than compen- covery would have on even a small relic density of sates for the dimished rate within UCMHs. The WIMPs in the Universe. Specifically, we consider abundance of minihalos also encodes information three discovery scenarios: 1) The detection of grav- about the evolution of the Universe prior to Big itational waves produced by the merger of subsolar Bang nucleosynthesis (BBN). Deviations from radia- BHs with LIGO/Virgo; 2) The detection of gravita- tion domination prior to BBN can enhance the mini- tional waves produced by the merger of O(10) solar halo poputation, thereby boosting the dark matter mass BHs at redshift z > 40 with the Einstein tele- annihilation rate within dwarf spheroidal galaxies if scope; 3) The detection of the radio emission pro- dark matter is a thermal relic. Conversely, the non- duced by the accretion of gas onto 1000 thermal production of dark matter can suppress the BHs with the Square Kilometer Array. We esti- small-scale power spectrum. It is therefore possible mate the abundance of PBHs in each scenario, and, to use gamma-ray observations and observations of from that, we calculate the gamma-ray luminosity the Lyman-α forest to learn about the origins of dark of WIMP overdensities around PBHs in the Milky matter and the evolution of the Universe during its Way. By comparing it with the observed diffuse first second. extragalactic gamma-ray flux and with unidentified gamma-ray point sources in the 3FGL Fermi cata- logue, we show that a positive detection of even a 124 — Galaxies small number of PBHs in any of the above scenar- ios would set extraordinarily stringent constraints 124.01 — What’s lighting up the Magellanic on weak-scale extensions of the Standard Model, in- Stream? cluding those predicting a WIMP abundance much Kat Barger1; Greg Madsen10; Andrew Fox2; Bart smaller than that of dark matter, ruling out almost P. Wakker3; David L. Nidever4; Lawrence Matthew the entire parameter space of popular theories like Haffner5; Jacqueline Antwi-Danso6; Mike Hernandez1; the so-called MSSM7, GUT-scale SUSY and scalar Nicolas Lehner7; Alex S. Hill8; Andrew curzons9; singlet scenarios. If time allows, I will also dis- Thorsten Tepper-garcia9; Jonathan Bland-Hawthorn9 cuss complementary constraints on the particle na- 1 Physics and Astronomy, Texas Christian University (Fort Worth, ture of dark matter arising from the analysis of stellar Texas, United States) streams. 2 University of Cambridge (Cambridge, United Kingdom) 3 Space Telescope Science Institute (Baltimore, Maryland, United 123.04 — The Early Universe’s Imprint on Dark States) Matter 4 University of Wisconsin-Madison (Madison, Wisconsin, United 1 1 1 States) Adrienne L. Erickcek ; M. Sten Delos ; Carisa Miller ; 5 Kayla Redmond1 Montana State University (Bozeman, Montana, United States) 6 Embry-Riddle Aeronautical University (Daytona, Florida, United 1 University of North Carolina at Chapel Hill (Chapel Hill, North States) Carolina, United States) 7 Texas A&M University (College Station, Texas, United States) 8 As remnants of the earliest stages of structure forma- University of Notre Dame (South Bend, Indiana, United States) 9 tion, the smallest dark matter halos provide a unique The University of British Columbia (Vancouver, British Columbia, probe of the density fluctuations generated dur- Canada) 10 ing inflation, the evolution of the Universe shortly Sydney Institute for Astronomy (Sydney, New South Wales, after inflation, and the origins and properties of Australia) dark matter. The absence of early-forming ultra- compact minihalos (UCMHs) establishes an upper Galaxy interactions have greatly disturbed and redis- bound on the amplitude of the primordial power tributed the gas in the Magellanic System through- spectrum on small scales and has been used to con- out the halo of the Milky Way. Using the Wiscon- strain inflationary models. Numerical simulations sin H-α Mapper (WHAM) telescope, we have com- of UCMH formation reveal that these constraints pleted the highest sensitivity and kinematically re- need to be revised because the dark matter annihi- solved emission-line survey of the entire Magellanic lation rate within UCMHs is lower than has been Stream. These observations enable us to determine assumed. Nevertheless, minihalos can still provide how the ionization conditions change over 100 de- unrivaled constraints on the small-scale primordial grees across the sky, including the region below the power spectrum because dark matter annihilation South Galactic Pole. We explore the sources of that ionization and find that photoionization from the

38 Milky Way and Magellanic Clouds is insufficient to 124.03 — Evidence in favor of Density Wave explain the observed H-α emission. We further in- Theory, through multiwavelength image analysis, vestigate whether halo-gas interactions, self ioniza- spatially resolved stellar clusters and star tion through a “shock cascade” that results as the formation history maps

Stream plows through the halo, and energetic pro- 1 1,2 cesses associated with the Milky Way’s center could Mohamed S. Abdeen ; Daniel Kennefick ; Julia D. Kennefick1,2; Rafael T. Eufrasio1,2 be responsible for the ionization. The gas in the Mag- 1 ellanic Stream could supply enough gas to maintain Department of Physics, University of Arkansas (Fayetteville, Arkansas, United States) or even boost the star formation in the Milky Way, 2 but only if it can survive the journey to the Galaxy’s Arkansas Center for Space & Planetary Sciences, Univ. of disk. Arkansas (Fayetteville, Arkansas, United States) Stationary density wave theory, originally proposed 124.02 — Multi-wavelength Study of Spiral by C.C. Lin and Frank Shu (Lin & Shu 1964), explains Structure and Star-Formation Region in Disk the nature and the origin of spiral arm structures in Galaxies galaxies as density waves which propagates through Ryan Miller1; Daniel Kennefick1; Julia D. Kennefick1; the galactic disk. It predicts the existence of an age Mohamed Shameer Abdeen1; Douglas Shields1; Ben- gradient across the spiral arm with a change in the jamin L. Davis2; Erik Monson1; Rafael T. Eufrasio1 age gradient direction at the co-rotation radius. Us- 1 Physics, University of Arkansas (Fayetteville, Arkansas, United ing an image overlaying technique we were able de- States) velop a method for identifying the co-rotation ra- 2 Swinburne University of Technology (Melbourne, Victoria, Aus- dius. By considering spatially resolved stellar clus- tralia) ters of different ages and by analyzing star formation history maps we have found compelling results in fa- The density-wave theory of spiral structure proposes vor of Density Wave Theory. We have derived star- that star formation occurs in or near a spiral-shaped formation history (SFH) maps with LIGHTNING region of higher density that rotates rigidly within (Eufrasio et al. 2017) spectral energy distribution the galactic disk at a fixed pattern speed. In most (SED) fitting procedure, which incorporated pho- interpretations of this theory, newborn stars move tometric data from GALEX, Swift, SDSS, 2MASS, downstream of this position as they come into view, Spitzer, WISE, and Herschel. The SFH were de- forming a downstream spiral which is tighter, with a rived non-parametric bins of 0–10Myr, 10–100Myr, smaller pitch angle than that of the density-wave it- 0.1–1Gyr, 1–5Gyr, and 5–13.6Gyr. The dynamic evo- self. Rival theories, including theories which see spi- lution of spiral arms can be traced by observing these ral arms as essentially transient structures, may de- stellar cluster maps and SFH maps. They can be mand that pitch angle should not depend on wave- quantified by tracing spiral arms, measuring pitch length. We measure the pitch angle of a large sample angles and also by observing the azimuthal offsets of galaxies at several wavelengths associated with relative to the dust lanes. 8µm, Infrared Spitzer im- star formation or very young stars (8.0 microns, H- ages were used as a tracer for dust lanes, hence de- α line and 151 nm in the FUV) and show that they picting the maximum intensity locations of the den- all have the same pitch angle, which is larger than the sity wave. pitch angle measured for the same galaxies at optical and NIR wavelengths. Our measurements in the B- 124.04 — (withdrawn) band and at 3.6 microns have unambiguously tighter This abstract was withdrawn. spirals than the star-forming wavelengths. In addi- tion, we have measured in the u-band, which seems to fall midway between these two extremes. Thus 124.05 — Low-Luminosity Core Dominated Radio our results are consistent with a region of enhanced Galaxies and the Extragalactic Gamma-Ray stellar light situated downstream of a star-forming Background region. Chris R. Shrader1,2; Floyd W. Stecker1; Matthew Arnold Malkan3 1 NASA’s GSFC (Greenbelt, Maryland, United States) 2 CUA (Washington, DC, District of Columbia, United States) 3 UCLA (Los Angeles, California, United States)

39 Recent surveys have revealed a large number of low- 124.07 — A WISE Determination of the luminosity core dominated radio galaxies that are Contribution of Galaxies to the Extragalactic much more abundant than those at higher lumi- Background Light at 3.4 μm

nosities. These objects will be too faint in gamma- 1,2 3 4 rays to be detected individually by Fermi. Neverthe- Sean E. Lake ; Edward L. Wright ; Roberto J. Assef ; Thomas H. Jarrett5; Sara M. Petty6; S. Adam Stanford7; less, they may contribute significantly to the unre- 8 1,2 solved extragalactic gamma-ray background (EGB). Daniel Stern ; Chao-Wei Tsai 1 National Astronomical Observatories of China (Beijing, China) We consider the possible contribution of this popula- 2 tion to the EGB. Using available data available for 45 CAS Key Laboratory of FAST, NAOC, Chinese Academy of Sci- ences (Beijing, China) radio galaxies listed as gamma-ray detected counter- 3 parts we have searched radio maps which can resolve Physics and Astronomy Department, UCLA (Los Angeles, Cali- fornia, United States) the core flux from the total source flux. We were able 4 to obtain core fluxes for virtually every source which Nùcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales (Santiago, Chile) we then used to derive a relation between core radio 5 flux and gamma-ray flux. We then extrapolated to Astronomy Department University of Cape Town (Cape Town, South Africa) low radio where the predominant pop- 6 ulation is apparently highly core dominated. Em- NorthWest Research Associates (Redmond, Washington, United States) ploying a very recent determination of the luminos- 7 ity function for core dominated radio galaxies we Department of Physics, UC Davis (Davis, California, United States) estimate the contribution of all possible gamma-ray 8 emitting radio galaxies to the unresolved extragalac- Jet Propulsion Laboratory, California Institute of Technology tic gamma-ray background. We find this contribu- (Pasadena, California, United States) tion to be a possibly non-negligible, 4% - 18%. The study of the extragalactic background light (EBL) in the optical and near infrared has received 124.06 — Dry/mixed galactic interactions do not a lot of attention in the last decade, especially near trigger star formation a wavelength of λ ≈ 3.5 µm, with remaining tension Jun-Sung Moon1; Suk-Jin Yoon1 among different techniques for estimating the back- 1 Department of Astronomy, Yonsei University (Seoul, Seoul, Korea ground. We use measurements of the mean spectral (the Republic of)) energy distribution (SED) and luminosity function of galaxies optimized for this purpose to produce We investigate star formation (SF) in interacting new estimates of the contribution of galaxies to the galaxies, focusing on the impact of neighbors. Galax- EBL at 3.4 µm using WISE W1 photometry. Our re- ies in pairs are selected from the Sloan Digital Sky sults are consistent with extant measures, though a Survey. We classify the pairs into two groups accord- little higher than most. The source of the tension is ing to the SF activity of the neighbor, namely (i) ones how the luminosity function and mean SED evolves with a quiescent neighbor and (ii) ones with a star- at high redshifts (z > 1). forming neighbor. We carefully build control sam- ples of isolated galaxies by matching the redshift, stellar mass, and local density. We find that SF of 125 — Solar Physics Division galaxies paired with a star-forming neighbor is more Meeting (SPD), Corona 2 enhanced than the control sample, consistent with other studies. More interestingly, however, we un- 125.01 — A Comprehensive Assessment of EUV expectedly find no enhancement of SF in interactions Polar Coronal Holes: 1996 — 2018 with a quiescent neighbor. This opposes the conven- 1 2 2 tional view that galactic interactions lead to bursts Michael S. Kirk ; W. Dean Pesnell ; Charles Arge 1 of SF. We propose that gas richness of neighbors is a Catholic University of America (Washington, District of critical factor for triggering SF even during the “pair” Columbia, United States) 2 stages of mergers. We discuss possible mechanisms NASA Goddard Space Flight Center (Greenbelt, Maryland, to explain the observed trends. United States) Polar Coronal Holes are the longest-lived features on the sun and are a critical piece to understand the global state of the solar corona. Because of the

40 oblique viewing angle, obstruction due to the coro- topological features, such as null points and quasi- nal plasma scale height, and lack of ground truth separatrix layers (QSLs), which are regions charac- make segmentation of polar holes difficult. We terized by high values of the squashing factor. We make new measurements of polar hole’s perimeter also identified evidence of magnetic reconnection at and area in three EUV wavelengths between 1996 such locations, which can produce favorable con- and 2018 using five different space-based imagers: ditions, e.g., density enhancement by compression SOHO EIT, STEREO A and B EUVI, PROBA2 SWAP, and/or mass trapping in plasmoids, that can trigger and SDO AIA. The generated time-series of coronal run-away radiative cooling. We will discuss the sig- hole parameters rarely agree with each other, which nificance and broader implications of these novel ob- presents a difficult data problem: multi-band, multi- servations. instrument, heteroscedastic measurements with pe- riodic and systematic signals. We combine these 125.03 — Fluxon Modeling of CMEs and the measurements using a parametric bootstrap method Steady Solar Wind to make an empirical estimation of the polar coronal 1 1 1 hole’s size, boundary, and center of mass. This tech- Chris Lowder ; Derek Lamb ; Craig DeForest 1 nique allows us to simultaneously analyze the physi- Southwest Research Institute (Boulder, Colorado, United States) cal properties of polar coronal holes and identify reg- ular periodicities in our data from other origins. We The Field Line Universal relaXer (FLUX) code pro- present a comprehensive view of the EUV polar coro- vides a framework for modeling the evolution of nal hole over the past 22 years. the solar coronal magnetic field through the use of fluxon structures. Each fluxon represents a piecewise-linear analogue for magnetic field lines, 125.02 — Coronal Condensation at Preferential and carries a finite quantity of magnetic flux. Ap- Topological Locations: The Birth of Solar propriate forces are computed and applied at vertex Prominences and Coronal Rain points along each fluxon, allowing for relaxation to Wei Liu1; Xudong Sun2; Sijie Yu3; Patrick Antolin4; an equilibrium state. For a given initial configura- Viacheslav Titov5; Cooper Downs5; Thomas Berger6 tion, this allows for the study of fieldline topology 1 Stanford-Lockheed Institute for Space Research (Palo Alto, Califor- and subsequent evolution. The nature of the FLUX nia, United States) model allows for enhanced efficiency when com- 2 University of Hawaii at Manoa (Pukalani, Hawaii, United States) pared with grid-based MHD models, and avoids nu- 3 New Jersey Institute of Technology (Newark, New Jersey, United merical reconnection issues. We describe recent en- States) hancements to the FLUX code, including work with 4 University of St Andrews (St Andrews, United Kingdom) data assimilation, calculation of steady solar wind 5 Predictive Science, Inc. (San Diego, California, United States) solutions, and CME eruption triggering. 6 University of Colorado (Boulder, Colorado, United States) 125.04 — The Correlation Between The Enhanced The million-degree hot and tenuous solar coronal Sulfur Abundance in Slow Solar Winds and The plasma, under certain conditions, can enigmatically Magnetic Field Geometry of Their Source Regions undergo a radiative cooling instability and condense into material of 100 times cooler in the form of promi- Natsuha Kuroda1; J. Martin Laming2 nences or coronal rain. Where, when, and how such 1 University Corporation for Atmospheric Research (Boulder, Col- cooling condensation takes place remain poorly un- orado, United States) derstood. Answers to these questions are not only 2 Naval Research Laboratory (Washington, District of Columbia, of scientific importance in their own right, but also United States) bear implications for the fundamental question of coronal heating and the chromosphere-corona mass We present an examination of the First Ionization Po- cycle. Magnetic fields in the magnetized corona tential (FIP) fractionation scenario by the pondero- undoubtedly play a crucial role (e.g., by trapping motive force in the chromosphere by using observa- the plasma), but where and how? We report re- tions from The Solar Wind Ion Composition Spec- cent imaging and spectroscopic observations from trometer (SWICS) on board The Advanced Compo- SDO/AIA/HMI and IRIS that can shed light on sition Explorer (ACE). Based on the prediction of the these puzzles. Through a systematic survey, we ponderomotive force model by Laming et al. (2019) found that a large fraction of quiet-Sun condensa- that the abundance enhancements of intermediate tions preferentially occur at the dips of coronal loops FIP elements, S, P, and C, in slow solar wind can or funnels. Such dips are located at/near magnetic be explained by the release of plasma from strong

41 open fields, much stronger than those usually asso- WSA model results, as well as the effects of both en- ciated with fast wind source regions, we examine the hancing and reducing the net flux in AR11087. We possible correspondence between the enhanced frac- also present a newly developed method for quanti- tionation of intermediate FIP elements in slow solar tatively ranking ADAPT map realizations based on winds and the magnetic field strength of their source well the ADAPT driven WSA predictions agree with regions. We do so by surveying the extensive record spacecraft observations. of solar wind speeds and composition from the ACE mission, and investigating the magnetic feature on 125.06 — Understanding uniturbulence: the Sun associated with the repeated sulfur abun- self-cascade of MHD waves in the presence of dance anomaly corresponding to the decrease in the inhomogeneities solar wind speed, found over about four solar rota- 1 1 tion cycles in the beginning of 2008. We also obtain Norbert Magyar ; Tom Van Doorsselaere ; Marcel 1 rough profiles of the magnetic field strength atthe Goossens 1 source regions of these slow winds, estimate the frac- Centre for mathematical Plasma Astrophysics, Department of tionation values of various elements using the pon- Mathematics, KU Leuven (Leuven, Belgium) deromotive force model with the field profiles as in- puts, and compare the results with the observed frac- It is a generally accepted fact in the MHD turbulence tionation values. community that the nonlinear cascade of wave en- ergy requires the existence of counter-propagating Alfvénic wave-packets, along some mean magnetic 125.05 — Quantitatively Comparing WSA Coronal field. This fact is an obvious outcome of theMHD and Solar Wind Model Predictions with equations when assuming an incompressible and ho- Observations Using ADAPT Input Maps mogenoeus plasma. There have been relatively few Charles Nickolos Arge1; Carl John Henney3; Shaela I. attempts to relax these assumptions in the context Jones1; Kathleen Shurkin3; Samantha Wallace2 of MHD turbulence studies. However, it should be 1 Solar Physics Laboratory, NASA/GSFC (Greenbelt, Maryland, clear that once these assumptions brake down, the United States) generally accepted picture of turbulent cascade gen- 2 University of New Mexico (Albuquerque, New Mexico, United eration is not universal. In the context of longitudi- States) nally stratified plasmas (i.e. gravitationally stratified 3 Air Force Research Laboratory (Albuquerque, New Mexico, coronal holes), it has been known since the 70’s that United States) inhomogeneities along the mean magnetic field lead to the linear coupling of sunward and anti-sunward Reliable estimates of the global solar photospheric propagating waves. This leads to co-propagating magnetic field distribution are critical to accurately disturbances of Elsasser fields, which can interact co- model and understand solar and heliospheric mag- herently to initiate a nonlinear cascade. The alter- netic fields. The Air Force Data Assimilative Pho- native case of perpendicular inhomogeneity (across tospheric flux Transport (ADAPT) model generates the mean magnetic field) was even less studied in synchronic (i.e., globally instantaneous) maps by the context of MHD turbulence. In this study we evolving observed solar magnetic flux using rel- show that these type of inhomogeneities lead also atively well understood transport processes when to co-propagating Elsasser fields, already in the in- measurements are not available and then updating compressible case. We show how the nonlinear self- modeled flux with new observations using data as- deformation of these unidirectionally propagating similation methods that rigorously take into account waves leads to a cascade in k-space across the mag- model and observational uncertainties. ADAPT has netic field. The existence of this type of unidirec- recently been upgraded so that it now uses reverse tional cascade might have an additional strong ef- active region (RAR) modeling, which is a process to fect on the turbulent dissipation rate of dominantly include active regions that emerged on the far-side of outward propagating Alfvénic waves in structured the Sun and smoothly evolve them forward in time plasma, as in solar coronal holes. onto the visible disk. This paper compares Wang- Sheeley-Arge (WSA) coronal and solar wind model- ing results at Earth and STEREO A & B using ADAPT RAR input model maps for the time interval of June- July 2010, when the active region (AR11087) emerged on the far-side of the Sun. Driven by global maps with and without RARs, we test the sensitivity of the

42 126 — Solar Physics Division as of the geometry of the plasma in the upper solar chromosphere. Meeting (SPD), Instrumentation CLASP2 will launch from White Sands Missile Range in April 2019. In this presentation, we will 126.01 — The Chromospheric Layer summarize the characteristics of the CLASP2 flight, Spectro-Polarimeter (CLASP2) Sounding Rocket the performance of the UV telescope and spectropo- Mission: First Results larimeter, and our preliminary findings. David Eugene McKenzie1; Ryohko Ishikawa2; Ryouhei Kano2; Laurel Rachmeler1; Javier Trujillo Bueno3; Ken 126.02 — The FOXSI-3 rocket: Overview and early Kobayashi1; Donguk Song2; Masaki Yoshida2; Frederic results of its latest flight 4 2 Auchere ; Takenori Okamoto 1 2 1 Juan Camilo Buitrago-Casas ; Lindsay Glesener ; NASA Marshall Space Flight Center (Huntsville, Alabama, Sasha Courtade1; Juliana Vievering2; Subramania Athi- United States) 3 2 4 2 ray Panchapakesan ; Sophie Musset ; Daniel Ryan ; National Astronomical Observatory of Japan (Tokyo, Japan) 1 5 3 Gregory Dalton ; Shin-Nosuke Ishikawa ; Noriyuki Instituto Astrofísica de Canarias (Santa Cruz de Tenerife, Spain) 6 3 5 4 Narukage ; Stephen Bongiorno ; Kento Furukawa ; Institut d’Astrophysique Spatiale (Paris, France) Lance Davis2; Paul Turin1; Zoe Turin7; Tadayuki Takahashi5; Shin Watanabe5; Sam Krucker1; Steven A major challenge for heliophysics is to decipher Christe4; Brian Ramsey3 the magnetic structure of the chromosphere, because 1 Space Sciences Lab, UC Berkeley (Berkeley, California, United of its vital role in the transport of energy into the States) corona and solar wind. Routine satellite measure- 2 University of Minnesota (Minniapolis, Minnesota, United States) ments of the chromospheric magnetic field will dra- 3 NASA Marshal Space Center (Huntsville, Alabama, United matically improve our understanding of the chro- States) mosphere and its connection to the rest of the solar 4 NASA Goddard Space Flight Center (Greenbelt, Maryland, atmosphere. Before such a satellite can be consid- United States) ered for flight, we must refine the measurement tech- 5 Institute of Space and Astronautical Science, Japan Aerospace niques by exploring emission lines with a range of Exploration Agency (Kanagawa, Japan) magnetic sensitivities. In 2015, CLASP achieved the 6 National Astronomical Observatory of Japan (Tokyo, Japan) first measurement of linear polarization produced by 7 Georgia Tech Research Institute (Atlanta, Georgia, United States) scattering processes in a far UV resonance line (hy- drogen Lyman-α), and the first exploration of the Hard X-rays (HXRs) from the solar corona are closely magnetic field (via the Hanle effect) and geometri- connected to energy releases and particle transport cal complexity in quiet regions of the chromosphere- in solar flares of all sizes. Expressly, faint solar HXR corona transition region. These measurements are a emissions are of remarkable interest in understand- first step towards routine quantitative characteriza- ing solar flare structure and dynamics. This is be- tion of the local thermal and magnetic conditions in cause of their connection with, for instance, loop top this key layer of the solar atmosphere. emission and small flares. Mainly due to the indirect Nonetheless, Lyman-α is only one of the mag- imaging methods used by past solar-dedicated HXR netically sensitive spectral lines in the UV spec- imagers, like RHESSI, faint HXRs observations have trum. CLASP2 extends the capability of UV spec- been limited by the imaging dynamic range and sen- tropolarimetry by acquiring ground-breaking mea- sitivity of the instruments. surements in the Mg II h and k spectral lines near The Focusing Optics X-ray Solar Imager (FOXSI) 280 nm, whose cores form about 100 km below the sounding rocket payload is the first solar-dedicated Lyman-α core. These lines are sensitive to a larger instrument designed for performing imaging spec- range of field strengths than Lyman-α, through both troscopy in the 4-20 keV range by using direct fo- the Hanle and Zeeman effects. CLASP2 will cap- cusing optics. FOXSI has successfully flown three ture measurements of linear and circular polariza- times from the White Sands Missile Range in New tion to enable the first determination of all 4 Stokes Mexico. For its latest rocket campaign (FOXSI-3), an parameters in chromospheric UV radiation. Cou- enhanced version of the experiment, which includes pled with numerical modeling of the observed spec- optics and detector upgrades, was implemented for tral line polarization (anisotropic radiation pump- the launch which happened on September 7, 2018. ing with Hanle, Zeeman and magneto-optical ef- In this talk, we present an overview of the FOXSI- fects), CLASP2 is a pathfinder for determination of 3 campaign, describing in detail the improved capa- the magnetic field’s strength and direction, as well bilities of the telescope and how they allow for better

43 investigation of faint coronal HXRs. We also present here is a detector concept that has been developed a preliminary analysis of the FOXSI-3 observations. as part of the NASA Innovation Advanced Concept program in 2018/19 and how it can be expanded 126.03 — Satellite mission: PhoENiX (Physics of upon to do Science. The basic idea is that by go- Energetic and Non-thermal plasmas in the X (= ing closer to the Sun the intensity of Solar Neutri- magnetic reconnection) region) nos will go up by factors of thousands, but in ad- dition to this a space-craft can go off the ecliptic 1 Noriyuki Narukage plane to view the Sun at high latitudes and even the 1 National Astronomical Observatory of Japan (Mitaka, Tokyo, polar region which could do unique studies of the Japan) that cannot be done on Earth. The Sun can also act as a Gravitational Lens with millions of We are studying a new solar satellite mission, time light collecting power and the Grav- ”PhoENiX”, for understanding of particle accelera- itational Lens which is much closer to the Sun at tion during magnetic reconnection, which are ubiq- 25 AU than the light Gravitational Focus is reach- uitous features exhibited by a wide range of plasmas able with current rocket launch technology. Other in the universe. The main observation targets of this than the Sun the largest neutrino source in the night mission are solar flares that are caused by magnetic sky would be the Galactic core and it can be imaged reconnection and accelerate plasma particles. The as a space craft transversing the Neutrino Gravita- sun is a unique target in the sense that it can be in- tional Lens focus to study the structure of the Galac- vestigated in great detail with good spatial, temporal tic core. There is even the possibility to study Dark and energy resolutions. The scientific objectives of Matter with a space-craft with a neutrino detector this mission are (1) to identify particle acceleration since solar neutrinos are a background and this back- sites, (2) to investigate temporal evolution of parti- ground could be changed as a flight trajectory takes cle acceleration, and (3) to characterize properties of the detector mounted space-craft to different solar accelerated particles, during magnetic reconnection, radii distances. These new ideas are under study to i.e., during solar flares. In order to achieve these sci- see the total science potential of such a program. ence objectives, the PhoENiX satellite is planned to be equipped with three instruments of (1) Photon- 126.05 — Photon sieves and the future of EUV counting type focusing-imaging spectrometer in soft imaging spectroscopy X-rays (up to ∼10 keV) demonstrated by FOXSI-3, (2) Photon-counting type focusing-imaging spectrome- Adrian N. Daw1; Douglas M. Rabin1; Donald James ter in hard X-rays (up to ∼30 keV) like FOXSI series, Schmit1; Kevin Denis1 and (3) Spectropolarimeter in soft gamma-rays (spec- 1 NASA Goddard Space Flight Center (Greenbelt, Maryland, troscopy is available in the energy range of from > United States) 20 keV to < 600 keV; spectropolarimetry is available from > 60 keV to < 600 keV) like Hitomi/SGD. We Large-aperture photon sieves fabricated at NASA- plan to realize this satellite mission around next so- GSFC can provide diffraction-limited imaging at lar maximum (around 2025). In this presentation, we EUV and X-ray wavelengths, that is, spatial scales will explain the details of science goal, science ob- down to milli-arcseconds, and are also being used jectives and instruments of PhoENiX mission. Addi- to provide monochromatic, collimated beams for tionally, in order to demonstrate the unprecedented the calibration of solar EUV instruments such as observations with PhoENiX, we will show the soft X- the Extreme Ultraviolet Normal Incidence Spectro- ray photon-counting data taken by FOXSI-3 sound- graph (EUNIS). EUNIS is a two-channel imaging ing rocket. spectrograph with unprecedented dynamic range and broad spectral coverage (9-11 nm and 52-64 nm), scheduled for a sounding rocket flight in September 126.04 — Science Mission of a Neutrino 2019. This will be the first time the 9-11 nm wave- Space-craft length range of the Sun has ever been observed by Nickolas Solomey1 an imaging spectrograph, despite the importance of 1 Physics, Wichita State University (Wichita, Kansas, United these short EUV/soft X-ray wavelengths to observ- States) ing the hottest (>5MK) plasma in the non-flaring at- mosphere, which is critical to understanding the en- The development of a Neutrino Detector that can ergization of the solar corona. Recent results will be be operated in Space would result in the ability to presented, and capabilities for future solar EUV mis- do several major science investigations. Presented sions will be discussed.

44 126.06 — TSMM - A Tomographic Solar 127 — George Ellery Hale Prize Magnetism Mission Lecture: Observations about Haosheng Lin1; Maxim Kramar1 1 Institute for Astronomy, Univ. of Hawaii (Pukalani, Hawaii, Observations of the Sun, Philip United States) Scherrer (Stanford University)

Detailed knowledges of the magnetic and thermal 127.01 — Observations about Observations of the environment of the solar atmosphere, including the Sun photosphere, chromosphere, and the corona, and how the plasma and the magnetic fields interact Philip H. Scherrer1 with each other, are crucial for the understanding of 1 Stanford Univ. (Stanford, California, United States) the physics of solar eruptions, which directly influ- ences space weather in interplanetary space. How- After more than 50 years as an observer of the Sun, ever, the inference of the 3D coronal vector magnetic of the process of observing the Sun, and of the peo- fields from observations is not straightforward due ple who participate in the adventure I will offer some to the complex nature of the emission process (reso- comments about what I have learned. nance scattering through Hanle and Zeeman effects) and line-of-sight (LOS) integration through the op- tically thin corona. Recent progresses in spectropo- 128 — iPoster Plus III: Dust & Star larimetric measurements of the polarized spectra Formation of magnetically sensitive corona emission lines and their interpretation, and the development of tomo- 128.01 — Spinning Dust Emission from graphic inversion techniques now provides a viable Circumstellar Disks and Its Role In Excess path toward quantitative characterization of the 3- Microwave Emission dimensional coronal temperature, density, and mag- 1 2 3 netic field structures. Lan Quynh Nguyen ; Thiem Hoang ; Vinh Nguyen ; 1 Tomographic inversion relies on observations of Grant James Mathews 1 the object under study from multiple sight lines. For Physics, University of Notre Dame (Notre Dame, Indiana, United earth-bound observers, tomographic inversion of States) 2 the static temperature, density, and magnetic fields Korea Astronomy and Space Science Institute, (Daejeon, South structures can be realized using pseudo tomographic Korea, Korea (the Republic of)) 3 observations due to the rotation of the sun. However, Hanoi National University of Education (Hanoi, Hanoi, Viet to resolve the temporal evolution of the structures Nam) of the solar atmosphere before, during, and after so- Electric dipole emission from rapidly spinning poly- lar eruptions, a space mission consisting of multiple cyclic aromatic hydrocarbons is widely believed to spacecraft deployed in deep space circumsolar or- be an origin of anomalous microwave emission, but bits is needed to observe the sun from many sight recently it has encountered a setback owing to the lines simultaneously. This paper describes recent noncorrelation of anomalous microwave emission progresses in tomographic inversion techniques, and with polycyclic aromatic hydrocarbon abundance an instrument development effort to develop com- seen in a full-sky analysis. Microwave observa- pact and high-performance instrumentation that will tions for specific regions with well-constrained poly- enable the deployment of a deep-space tomographic cyclic aromatic hydrocarbon features would be cru- solar magnetism mission in the near future. cial to test the spinning dust hypothesis. In this paper, we present physical modeling of microwave emission from spinning polycyclic aromatic hydro- carbons from protoplanetary disks around Herbig Ae/Be stars and T Tauri stars where polycyclic aromatic hydrocarbons features are well observed. Guided by the presence of 10 μm silicate features in some protoplanetary disks, we also model mi- crowave emission from spinning nanosilicates. Ther- mal emission from big dust grains is computed us- ing the Monte Carlo radiative transfer code. Our

45 numerical results demonstrate that microwave emis- and a telescope. The starshade imaging charac- sion from either spinning polycyclic aromatic hy- teristics include both the diffraction from an ideal drocarbons or spinning nanosilicates dominates over or perturbed starshade as well as solar glint from thermal dust at frequencies ν < 60 GHz, even in the the starshade edges, the largest source of local in- presence of significant grain growth. Finally, we at- strument scatter. The telescope model assumes an tempt to fit millimeter-centimeter observational data ideal telescope with a user-defined obscured pupil with both thermal dust and spinning dust for sev- (e.g. secondary obstruction and struts). It incorpo- eral disks around Herbig Ae/Be stars that exhibit rates a vanilla detector model with read noise and polycyclic aromatic hydrocarbon features and find dark current. Finally, the astrophysics scenario in- that spinning dust can successfully reproduce the corporates Keplerian orbits, phase angles, geometric observed excess microwave emission. Future radio , different atmospheric scattering/absorption observations with ngVLA, SKA, and ALMA Band 1 laws, any kind of host star (by default the user can would be valuable for elucidating the origin of excess choose among any of the +10,000 stars from ExoCat) microwave emission and potentially open a new win- and a large variety of extragalactic background fields dow for probing nanoparticles in circumstellar disks. (galaxies, Quasars). Exodust emission is accurate for a solar system and flexible for an arbitrary user- 128.02 — A Comparison between Magnetic Field defined profile. As a result, it can virtually builda Directions Inferred from Planck and Starlight large variety of extra-solar systems with an arbitrary toward Gould Belt Clouds number of exoplanets of multiple types and any host star, adding an optional background field, to obtain 1 1 Qilao Gu ; Hua-bai Li a series of images throughout the proposed mission. 1 Physics, The Chinese University of Hong Kong (Hong Kong, and parallax are also taken into ac- Hong Kong) count when background fields are added to the sim- ulated images. There are default systems, like the We compare the magnetic field (B-field) orientations Solar System at any distance from us. We have em- inferred from Planck 353 GHz thermal dust polar- ployed the tool to support WFIRST-S, HabEx, and ization and starlight polarimetry data and study the other mission probe studies and ground telescope cloud-field alignment based on these two tracers concepts. within Gould Belt clouds, which show good agree- ment with each other. Furthermore, we analyze two fundamentally different alignment studies—global 130 — iPoster Plus V: Cosmology ( cloud scale, ∼ 10-100 pc) cloud-field alignment, which compares mean fields and global cloud ori- & Related Topics entations, and local ( pixel size scale, ∼ 0.1-1 pc) structure-field alignment, which compares this rela- 130.01 — Local IGM/CGM Diffuse Emission tion pixel by pixel—and find the connection between Constraints with HST+COS them. Steven V. Penton1,2 1 University of Colorado @ Boulder (Boulder, Colorado, United 129 — iPoster Plus IV: Extrasolar States) 2 LASP (Boulder, Colorado, United States) Planets The Cosmic Origins Spectrograph (COS) onboard the Hubble Space Telescope (HST) has observed 129.01 — SISTER: Starshade Imaging Simulation thousands of Lyman-α (Lyα) forest absorbers with Toolkit for Exoplanet Reconnaissance both the G130M grating (0< z < 0.19) and the G160M Sergi R. Hildebrandt1,2; Stuart Shaklan1; Margaret C. grating (0.14 < z < 0.48). In this research, we use Turnbull3,1; Eric Cady1 the 2D nature of the COS FUV MCP detectors to 1 Jet Propulsion Laboratory (Pasadena, California, United States) constrain the Lyα emission associated with Lyα ab- 2 Caltech (Pasadena, California, United States) sorbers. We will divide our Lyα absorber sample 3 SETI Institute (Madison, Wisconsin, United States) based upon proximity to the closest known galaxy to differentiate emission between intergalactic (IGM) We have developed a suite of software forming an and circumgalactic (CGM) regions. We will discuss end-to-end starshade imaging tool that produces im- the limits of these constraints/detections in terms of ages of an arbitrary user-defined exoplanetary sys- both cosmological implications and from a techno- tem and background as observed by a starshade logical standpoint of a future mission.

46 130.02 — Constraints on the intensity of 131 — iPoster Session: Education intergalactic magnetic fields with gamma-ray and radio observations of BL Lac-type blazars & History

Manel Errando1; Wenlei Chen2; James Buckley1; 131.01 — Precession Resolution Would Realize Francesc Ferrer1 Equinox 1 Washington University in St Louis (St. Louis, Missouri, United 1 States) Steve Durst 1 2 University of Minnesota (Minneapolis, Minnesota, United States) International Lunar Observatory Association (ILOA) (Kamuela, Hawaii, United States) The observed magnetic fields in galaxies and galaxy clusters are believed to result from dynamo ampli- The arrival and ascendance of the Aquarius Equinox fication of weak magnetic field seeds whose ori- Epoch continues to be widely considered and calcu- gin remains a long-standing open question. These lated using Earth Precession analytics. With the ap- seed magnetic fields will still be present in the in- proach to J2000.0 / New Millennium from the 1960s tergalactic medium. Beams of TeV gamma-rays from / 1970s especially, astrophysics and sci- blazar jets can be used to infer the intensity, coher- entists have been focusing intensely on Earth Preces- ence length, and helicity of the intergalactic mag- sion rates and expressions. The science community netic field. Intergalactic magnetic fields deflect the interest in what Copernicus called ’Earth’s 3rd Mo- electron- pairs produced by TeV gamma- tion’ has been complemented by the rise of public rays from blazars, resulting in broadened beams interest in precessional archeoastronomy. of secondary GeV gamma-rays known as pair ha- Work on Precession and Rotation of the Earth los. Such pair-cascades develop along the projected has accelerated since 1930, when the 88 constella- direction of the blazar jet, which is known from tions and their boundaries – fixed by Delporte along imaging radio observations. We present a novel strict lines of and as search for for GeV pair haloes that combines Fermi- they existed at epoch 1875.0 – finally became rati- LAT gamma-ray data around 12 high-synchrotron- fied and published by the International Astronom- peaked BL Lacs with well-determined jet orientation ical Union (IAU). Notable studies include, Lieske, from VLBA radio observations. Our study exploits IAU 1976 Precession Model (1977); Williams, Carto- the expected asymmetry of blazar pair haloes and graphic Coordinates and Rotational Elements (1994); uses advanced simulations of the pair cascades to im- Capitaine, IAU2000 Precession-Nutation Model and prove the sensitivity of previous studies and increase IAU2006 Precession Possible Upgrade (2017); Math- the signal to noise. Although we find no significant ews, IAU2000A/B (2002); Fukushima, A New Pre- detection, a 2σ hint for an extended pair halo along cession Formula (2003); Zhu, Earth Rotation Param- the direction of the jet appears in the stacked gamma- eters from VLBI (2017). ray data, corresponding to an intergalactic magnetic This work on higher rotation / precession accu- field with strength of about 10−15 Gauss. We will racy may help more precisely determine the appar- present the results of our analysis and discuss the ent arrival of the Sun on the ecliptic in the constella- limitations of pair-halo searches due to astrophysi- tion of Aquarius at the time of the March equinox, cal uncertainties. Finally, assuming that the appar- which is now calculated about 2597 AD using the ent convergence on B ∼ 10−15 G is not coincidental, IAU 1928 / current sky map. and we will outline a clear path towards a positive de- their boundaries are the results ultimately of hu- tection of blazar pair haloes with future space-borne man decision, as psychologist / polymath Carl Jung and ground-based gamma-ray observatories. noted in 1940 when first referencing the approach of the Aquarius equinox epoch. A Resolution by 130.03 — (withdrawn) the IAU General Assembly updating the Aquarius- Pisces constellation boundary for greater preces- This abstract was withdrawn. sional accuracy and human inclusivity could place the arrival of the Sun at the March equinox in con- stellation Aquarius in 2000 AD, to the great advance- ment for Astronomy, the IAU, and Humanity.

47 131.02 — When Will It Be...U.S. Naval adopted class clickers were not a component of the Observatory Daylight Savings Time Calculator original instructor’s syllabus and so were not ini-

1 1 tially used. Both classes experienced identical ques- Mark Thomas Stollberg ; Malynda Chizek-Frouard ; tions/prompts and were given the same amount Cross Ziegler2; Teresa Wilson1; Jennifer L. Bartlett1 1 of time to consider and respond to the prompts. U. S. Naval Observatory (Washington, District of Columbia, Students in the non-clicker class were encouraged United States) 2 to write responses in their notes and volunteers University of Maryland (College Park, Maryland, United States) were solicited to verbally contribute responses. Stu- dents in the clicker class were required to respond ”Spring forward, fall back” is a memory aid that and after each question saw histograms of the re- everyone uses to switch their clocks onto and sponses of their peers. The two classes continued off of Daylight Saving Time (DST) each year. in this way until the first exam, about 4-5 weeks But who can remember when DST starts and into the semester. Results from the first exam ends? Why do we do this at all? The U.S. showed the clicker-class averaging nearly 10 percent- Naval Observatory (USNO) now has an on-line age points higher than the non-clicker class (75.45 DST calculator (https://aa.usno.navy.mil/data/ vs. 65.66), a difference with statistical significance docs/daylight_time.php) and an updated informa- and strong effect (Z=4.31). For ethical reasons this tion page (https://aa.usno.navy.mil/faq/docs/ result prompted the instructor to immediately intro- daylight_time.php) to answer those questions. The duce clickers into the non-clicker class. Two subse- calculator uses The Uniform Time Act of 1966 and quent exams in each class showed no statistically sig- its subsequent revisions (1974, 1986, and 2005) to al- nificant differences in the class averages (77.56 vs. low a user to find the beginning and ending dates 77.50 and 79.56 vs. 77.90; Z=0.03 and Z=0.83 respec- for DST in the U.S. from 1967 to 9999; calculations tively). This dramatic turnaround in performance for future years assume the current rules remain of the non-clicker class suggests that the students’ in effect. Users may also access this web calcula- physical act of responding to prompts with clickers, tor via an Application Programming Interface (API), and seeing the responses of their peers, was respon- which enables them to use the output in their own sible for the improvement. applications. Documentation for using all USNO API-enabled calculators, including sample calls, is also available online (https://aa.usno.navy.mil/ 131.04 — The Cold Case of SN1054. Was it the data/docs/api.php). First Cover-up in the History of Astronomy? Jeffrey L. Payne1; M.D. Filipovic1; Giuseppe Longo2; 131.03 — Clickers in the Classroom: Dramatic Thomas H. Jarrett4; Miro Ilic3; Jordan Collier1; Nicholas Results from an Accidental Experiment Tothill1; Evan Crawford1 1 Western Sydney University (Sydney, New South Wales, Aus- Stephen J. Kortenkamp1; Byron Hempel1 tralia) 1 University of Arizona (Tucson, Arizona, United States) 2 University Federico II (Napoli, Italy) 3 Advocates for the use of clickers in university STEM Trebinje Astronomical Association (Srpska, Bosnia and Herzegov- ina) classes can find support in studies comparing en- 4 gagement and performance of students in similar University of Cape Town (Cape Town, South Africa) courses taught by different instructors who either We investigate the possible causes for missing his- use or do not use clickers. However, distinguish- torical records of the Supernova SN1054 in Europe. ing effects of clicker use from those due to different First, we establish that the previously acclaimed instructors can be challenging. Here we report re- “Arabic” records from Ibn Butlan originate from Eu- sults from an accidental experiment that arose due rope. As one of the most prominent scientists of the to an unforeseen leave of absence of an instructor time, he was in Constantinople at the time of the just one week into a semester. The orphaned class event and actively participating in the Church feud. was adopted by another instructor (SJK) who was al- Secondly, we reconstruct the European sky at the ready teaching a different section. Thus, the exper- time and find that the new “star” (SN1054) was in the imental setting involved the same instructor teach- west while the planet Venus was on opposite sides ing two sections of an introductory planetary sci- of the sky (in the east) with the Sun sitting directly ence course with the same lectures/activities. The between two equally bright objects, as documented fundamental difference? One class used clickers in East-Asian records. We find a striking similar- from the beginning of the semester while with the ity to this picture in specially minted coins printed

48 in Byzantium during this period. On these coins of show that the HZ for complex aerobic life is likely limited edition, we suggest that the Emperor’s head limited relative to that for microbial life. We use at the time, Constantine IX, might represent the Sun 1-D radiative-convective climate and photochemical with two “stars” on each side – Venus in the east and models to circumscribe a Habitable Zone for Com- SN1054 in the west, perhaps representing the newly plex Life (HZCL) based on known toxicity limits for split Christian churches. We suggest the east star a range of organisms as a proof of concept. We find points to the “stable” and well-known planet Venus that for CO2 tolerances of 0.01, 0.1, and 1 bar, the representing the Eastern Orthodox church and the HZCL is only 21%, 32%, and 50% as wide as the con- other new (and expected to be short-lived) Western ventional HZ for a Sun-like star, and that CO concen- Catholic church is represented by the new and fad- trations may limit some complex life throughout the ing star. We examine 29 coins of this rare Constan- entire HZ of the coolest M dwarfs. These results cast tine IX Class IV batch and found that their stars are new light on the likely distribution of complex life in gradually fading in size by ∼35% (or 1.50±0.25 mm). the universe and have important ramifications for the This change in star size across the Class IV coin sam- search for exoplanet and technosigna- ple could reflect the real situation on the sky where a tures. This research was supported by the NASA similar rate of change in SN1054 Astrobiology Institute Alternative Earths team un- is estimated (mv ∼1.4 mag) over the last six months der Cooperative Agreement Number NNA15BB03A of Constantine IX rule at the time when these coins and the NExSS Virtual Planetary Laboratory un- were minted. While knowledge and understanding der grant number 80NSSC18K0829. A preprint of of sky events (such as SN) were very poor in the mid this work can be found at https://arxiv.org/abs/ XI century, we argue that the Great Schism played 1902.04720. an essential role in turning aside the reporting of this very obvious event on the European sky. Finally, we propose that engravings on tombstones (stećci) from 200 — Laboratory Astrophysics several necropolises in today’s Bosnia and Herzegov- Division Plenary Lecture: The ina (far away from the Church’s influence) represent another true European record of the SN1054 event. Role of Dust in the Molecular Universe, Xander Tielens (Leiden 131.05 — A Limited Habitable Zone for Complex Life University, The Netherlands)

Edward Schwieterman1; Christopher Reinhard2; 200.01 — The Role of Dust in the Molecular Stephanie Olson3; Chester Harman4; Timothy Lyons1 Universe 1 University of California, Riverside (Riverside, California, United 1,2 States) Alexander Tielens 1 2 Georgia Institute of Technology (Atlanta, Georgia, United States) Leiden Observatory (Leiden, Netherlands) 2 3 University of Chicago (Chicago, Illinois, United States) Astronomy Department, University of Maryland (College Park, 4 NASA Goddard Institute for Space Studies (New York, New York, Maryland, United States) United States) Astrobiology, the study of emergence of life and the The habitable zone (HZ) is commonly defined as its distribution in the Universe, addresses the most the range of distances from a host star within which fundamental questions in science: ”How does life be- liquid water, a key requirement for life, may ex- gin ?” and ”Are we alone ?” Over the last 20 years, ist at a planet’s surface. Substantially more CO2 we have discovered that planets are bountiful in the than present in Earth’s modern atmosphere is re- galaxy and that one in every five solar-type stars has quired to maintain clement temperatures for most a planet in the habitable zone. We have learned that of the HZ, with several bars required at the outer have spread to essential every niche – edge. However, most complex aerobic life on Earth even the seemingly most inhospitable ones – on our is limited by CO2 concentrations of just fractions of a planet. And we have learned that life started essen- bar. At the same time, most exoplanets in the tradi- tially as soon as conditions permitted, within some tional HZ reside in proximity to M dwarfs, which are 200 million of the late heavy bombardment, or per- more numerous than Sun-like G dwarfs but are pre- haps even earlier. This has resulted in a paradigm dicted to promote greater abundances of gases that shift from ”Life on Earth is unique” to the premise can be toxic in the atmospheres of orbiting planets, ”life is widespread”. As a result, searching for pre- such as carbon monoxide (CO). In this poster, we biotic molecules in space that may jump start life

49 on nascent planets has taken on a life by itself. In 201.02 — Circumstellar Dust around Mira this talk, I will summarize this shift in our think- Variables and the Importance of Maser Emission ing and the global processes that may have influ- Lisa Shepard1; Angela Speck1 enced the first astrochemical steps in space. The fo- 1 cus in this talk will be on – the start- Physics & Astronomy, University of Missouri (Columbia, Mis- ing point of astrobiology – the chemical evolution souri, United States) that takes place in space where simple molecules Asymptotic Giant Branch (AGB) stars are major con- are transformed into complex molecules and com- tributors of to the interstellar medium. plex molecules are broken down to simple ones. This Understanding the formation of cosmic dust ejected chemical dance of the elements produces a wide va- from these stars is essential to understanding the riety of organic compounds. I will review the pro- broader topics of evolution and composition of stel- cesses that drive this chemical evolution in space, lar and interstellar objects in our universe. We inves- particularly in regions of star and planet formation. tigate the formation of circumstellar dust by study- The focus will be on understanding the raw materials ing the relationship between maser emission and that are delivered to newly formed planets and their dust spectral features for a sample of Mira variables. relationship to the building blocks from which pre- This project requires investigating the infrared spec- biotic material was formed and biological systems tra of a sizeable sample of stars for which maser evolve with an emphasis on the role of dust in this emission has been quantified. Using high-resolution chemical evolution. space-based spectroscopy data along with ancillary data from the published literature, we determine 201 — Star Formation, ISM and the nature of dust grains around these stars. This is achieved using two separate but complimentary Related Topics Poster Session methods. First, we match the positions and widths of observed spectral features with those seen in lab- 201.01 — Constraints on Large Scale Fluctuations oratory spectra. This is achieved by modeling the in the Galactic Magnetic Field star as a blackbody, which is subtracted from the ob- served spectrum to leave a residual dust-only spec- Steven R. Spangler1; Allison H. Costa2 trum. Then we fit a continuum to the dust only spec- 1 Univ. of Iowa (Iowa City, Iowa, United States) tra and divide to obtain the emission efficiency Q of 2 University of Virginia (Charlottesville, Virginia, United States) the observed spectral features. These are then com- The Galactic magnetic field consists of a large-scale, pared to laboratory spectra of potential astrominer- ordered component and turbulent fluctuations with als. The second method determines the composition a range of spatial scales. Values for the outer scale of the dust shell star using radiative transfer model- and amplitude of the fluctuations are uncertain. We ing. The dust shell parameters that result from these discuss a novel method for measuring or limiting analyses will then be compared to the parameters of fluctuations on size scales of order 30-50 . The maser emission to determine whether trends exist. method uses Faraday rotation measurements (rota- Here we present the first results of modeling the dust tion measure or RM) for lines of sight from back- composition. ground radio sources through HII regions. Costa and co-workers (ApJ 821,92,2016; 865,65,2018) report 201.03 — Investigation of Mid-infrared Dust RMs on 20-30 lines of sight through (or close to) each Spectral Features of Oxygen-rich AGB Star of two HII regions, the Rosette Nebula and W4. In Brian Hybben1; Angela Speck1 both cases, the RMs are dominated by the HII region, 1 University of Missouri (Columbia, Missouri, United States) and are consistent with the sign of the large scale Galactic field in that direction. This demonstrates Understanding cosmic dust and its origins furthers that the polarity of the magnetic field in a sphere understanding into the evolution of stellar objects with radius 15-20 parsecs centered on the HII region in the universe. Asymptotic Giant Branch (ABG) is the same as the large-scale field at that location. stars, being major contributors to the interstellar dust A model-dependent analysis of these results limits through their mass ejections, offers an opportunity the amplitude of the in-plane magnetic fluctuations to study and the impact of dust on to 50 - 70 % of the mean field. Future extensions of its environment. We have investigated the oxygen- the method will be discussed. rich Mira R Cas via radiative transfer modeling and infrared spectroscopic observations,

50 taken with the Infrared Space Observatory (ISO), and the Boston University Five College Radio Astron- the Infrared Astronomical Satellite (IRAS). Using omy Observatory Galactic Ring Survey (Jackson et DUSTY, a 1-d radiative transfer code, we have cre- al. 2006), toward YBs in order to determine molecu- ated models of the cosmic ejector from this AGB star. lar cloud velocities. Distances to these clouds were Because radiative transfer modeling is inherently de- then computed using a Bayesian distance calcula- generate, we sought ways to constrain the model in- tor that considers kinematic distance, displacement put variables. Using previously determined stellar from the galactic plane, and proximity to individ- parameters, such as mass-loss rate and expansion ve- ual parallax sources (Reid et al. 2016). Associa- locity for R Cas, we estimate the condensation tem- tions of YBs with dense clumps in the Hi-Gal cata- peratures for various potential astrominerals. Us- logue (Elia et al. 2017) and 2D Gaussian modeling ing the published photometric data to constrain the of the Spitzer 8- and 24-micron emission enabled us visible and near-infrared portions of the star’s spec- to determine critical physical properties of these ob- tral energy distribution, we aimed to match the ob- jects. We find compelling evidence that YBs are com- served spectroscopic data and determine to composi- pact star-forming regions spanning several orders of tion and density of the dust surrounding R Cas. Here magnitude in luminosity and occupying a relatively we present preliminary models of the dust composi- short transitional phase, when stellar content is first tion and discuss the methodologies for constraining revealed, but the surrounding ISM remains relatively model parameters. undisturbed. Thus, YBs are critical targets for stud- ies relating stellar content to the initial conditions for 201.04 — The Milky Way Project: Probing Star star formation. Formation with a New Yellowball Catalog 201.05 — Analyzing the Velocity Structure of the Grace A. Wolf-Chase1; Charles R. Kerton3; Kathryn 4 4 4 Young Protostellar Disk and Collapsing Envelope E. Devine ; Johanna Mori ; Leonardo Trujillo ; Sarah Around L1527 Schoultz4; Tharindu K. Jayasinghe2; Matthew S. Povich5 1 Adler Planetarium (Chicago, Illinois, United States) Brandon Alexander Hilliard1; Susan Terebey1,2 2 Ohio State University (Columbus, Ohio, United States) 1 Physics and Astronomy, California State University Los Angeles 3 Iowa State University (Ames, Iowa, United States) (Pasadena, California, United States) 4 The College of Idaho (Caldwell, Idaho, United States) 2 Jet Propulsion Laboratory (Pasadena, California, United States) 5 California State Polytechnic University (Pomona, California, United States) The life of a protostar begins in a giant of gas and dust, as a dense cloud core. After The Milky Way Project (MWP; Simpson et al. 2012) the dense core becomes self-gravitating it begins to is one of nearly 100 active research initiatives in collapse. If pressure and gravity are the dominant Zooniverse (zooniverse.org), the world’s largest on- forces then angular momentum will be conserved. line platform for citizen science. MWP participants The collapse quickly leads to a morphology that in- serendipitously discovered features they dubbed cludes a protostar, low-mass disk, infalling envelope, “yellowballs” (YBs) while searching Spitzer images and outflow cavity. The advent of ALMA means that for infrared “bubbles,” which are characteristic of the velocity of the infalling gas is now measurable. HII regions. Working with a small sample of YBs for In this study, the trajectories of collapsing material which distance estimates were available via associa- (infalling with rotation) toward the central mass will tion with catalogued Red MSX Source (Lumsden et be visualized along line of sight velocities by imple- al. 2013) survey objects, Kerton et al. (2015) argued menting rotational kinematics and thereby used to that YBs are young, compact photo-dissociation re- model the structure for different protostar sources. gions associated with intermediate and massive star Visualizing the motion of the material both in the formation. The current YB catalog contains over midplane of the disk and outside this region will also 6,000 objects, and includes the GLIMPSE/MIPSGAL be vital in creating a holistic model that can be com- inner galactic plane legacy surveys (Benjamin et al. pared with data from ALMA. The motion of the gas 2003; Churchwell et al. 2009; Carey et al. 2009), the and dust, during the earliest stages of the protostar’s Cygnus-X legacy survey (Beerer et al. 2010; Hora evolution, will be fundamental in determining how et al. 2007), and the Spitzer Mapping of the Outer the develops, and reveal key physical and Galaxy (SMOG; Carey et al. 2008) legacy survey. chemical characteristics. This investigation will dis- Here, we present results of a pilot study of 368 YBs cuss how the velocity structure model can be im- in the 30-40-degree longitude range of the galactic proved, and demonstrate simulated protostar data plane. We extracted 13CO spectra, obtained from

51 in relation to the well-known model of an edge-on history than other dwarf satellite galaxies of simi- source, namely the protostar L1527. lar mass. In larger satellite galaxies the gas is re- tained longer, and this allows star formation to con- 201.06 — Radial Velocity Monitoring of the Young tinue. The star formation history of Carina suggests Star Hubble 4 that it was once more massive, and has been trun- cated by the gravitational forces of the Milky Way or 1 1 Adolfo Carvalho ; Christopher M. Johns-Krull ; Lisa A. some other satellite. Gaia data provides precise pho- 2 Prato tometry, proper motions, , and positions 1 Physics and Astronomy, Rice University (Houston, Texas, United for over one billion stars. The proper motion and States) parallax data are especially intriguing, as measure- 2 Lowell Observatory (Flagstaff, Arizona, United States) ments of such precision were not previously avail- able for most of the stars. We selected potential mem- We have been spectroscopically monitoring the bers of Carina based on proper motion and posi- young star Hubble 4 for approximately 10 years us- tion in the color-magnitude diagram over an area ing the 2.7 m Harlan J. Smith telescope at McDonald of the sky ∼6.5 degrees across, and used these stars Observatory. Our goal is to monitor this star’s radial to search for low-surface-density indications of tidal velocity (RV) variations, and we have collected over interaction, such as non-axisymmetric distortions of 65 observations of this 2-3 Myr old T Tauri star. In the outer regions of Carina or extended tails along addition, we analyze archival imaging of Hubble 4 the direction of orbital motion that would indicate obtained with the ACS instrument aboard the Hub- tidally-removed stars. This project has been sup- ble Space Telescope to measure the flux ratio between ported by funding from National Science Foundation the members of this binary system. The RV measure- grant PHY-1560077. ments of Hubble 4 clearly reveal the long period (∼9 yr) variations due to the orbit of this binary (semi- 202.02 — Analysis of the RR Lyrae variable major axis of 5.6 AU) as well as much shorter period population in DDO216 (∼1.5 d) variations due to stellar rotation. By fitting and removing the variations due to orbital motion, Eleanor Stuart1; Ata Sarajedini1; Jillian R. Neeley1 we also find lower bound of ∼5 yr on the lifetime of 1 Physics, Florida Atlantic University (Fort Lauderdale, Florida, star spots on the surface of the star. We discuss the United States) implications of these findings for RV searches aimed at detecting planets around young stars. RR Lyrae (RRL) variable stars are some of the old- est stars in the universe and are widely used to gain insight into the properties of their host populations. 201.07 — (withdrawn) They are straightforward to locate due to their pe- This abstract was withdrawn. riodic variability and are used as a standard candle because their luminosities can be predicted from ob- servable quantities such as the period. In this study, 202 — Galaxies & Galaxy we identified and characterized RRL in the dwarf Evolution Poster Session galaxy DDO216, using archival Hubble Space Tele- scope (HST) observations. We identified about 1200 202.01 — A Search for Tidal Tails in the Satellite RRL candidates and used software to fit light curve Galaxy Carina templates to the data before manually evaluating the fit of each one and selecting about 150 RRLs thatfit Sean MacBride1,2 the templates well. From there, we plotted a Bailey 1 Physics, Wheaton College (Burlington, Vermont, United States) diagram and a color-magnitude diagram to examine 2 Rutgers University-New Brunswick (New Brunswick, New Jer- their amplitudes, periods, temperatures, and lumi- sey, United States) nosities. The preliminary Bailey diagrams follow the expected shape, with separate groups indicating ab- We searched for evidence of tidal stripping in the type and c-type RRLs, and the HR diagram shows spatial structure of the dwarf satellite galaxy Carina RRLs in their predicted location on the horizontal using data from the European Space Agency satel- branch. Individual for the RRL were cal- lite Gaia. The satellites of our Milky Way Galaxy culated based on a period-metallicity relation, and are remnants of clues to its birth. Carina is intrigu- we use a period-Wesenheit-metallicity relation to cal- ing because it has a more extended star formation culate the distance to DDO216. Once these proper- ties of the RRLs have been analyzed, further research

52 into the composition and evolution of DDO216 can used IRAF to determine the ellipticity and major- be conducted, which will allow us to better under- axis position angle in order to deproject the galaxy stand the evolution of dwarf galaxies. image to face-on. A two-dimensional Fast Fourier Transform was then applied to the deprojected im- 202.03 — Searching for Intermediate Mass Black age in order to measure the spiral arm pitch angle Holes in Spiral Galaxies Using Pitch Angles and, thereby, provide a SMBH mass estimate. We Gathered by Citizen Scientists compared this preliminary result of the black hole (BH) mass in NGC 4151 galaxy with the BH mass 1 2 1 Patrick M. Treuthardt ; Asher Scott ; Ian B. Hewitt has been estimated from seven independent tech- 1 North Carolina Museum of Natural Sciences (Raleigh, North niques (stellar dynamics, gas dynamics, reverbera- Carolina, United States) tion mapping , MBH-σ*, MBH-Vrot, MBH-n, MBH- 2 University of North Carolina (Chapel Hill, North Carolina, Lbulge, and MBH-P relation). We found the mass United States) values for the different techniques are in reasonable agreement with the recent estimate from stellar dy- We introduce Spiral Graph, a citizen science project namics, gas dynamics, and reverberation mapping dedicated to estimating the mass (M) of black holes techniques. Key words: supermassive black hole– (BHs) found in the nuclei of spiral galaxies. The main spiral galaxy- bulge luminosity – dispersion velocity- goal of this project is to identify intermediate mass 2 5 rotation velocity – pitch angle. black hole (IMBH; 10 M⊙ < MBH < 10 M⊙) candi- dates in an initial, stellar-mass complete sample of 202.05 — Selection Bias and Error Analysis in the 6222 spiral galaxies. To date, few confirmed IMBHs measured properties of Spiral Galaxies out to have been identified and the discovery of any new Redshifts of 2 candidates may provide much needed clues to the evolutionary history of more common supermassive Jonah Keller1 5 1 BHs (MBH > 10 M⊙) and their host galaxies. Physics, University of Arkansas, Fayetteville (Fayetteville, Utilizing the Zooniverse platform, we developed Arkansas, United States) a set of workflows for Spiral Graph that makes use of Recently, evidence has been presented for a strong the MBH – spiral arm pitch angle (PA) relationship to estimate central BH mass. Volunteers are tasked correlation between the mass of central black holes with fitting ellipses to the outer isophotes of galaxies and spiral arm pitch angles in local disk galaxies so that they may be deprojected to a face-on view. (Berrier et al., 2013). This implies an easier and more They are asked if each galaxy in question is indeed a effective method for determining central black hole spiral galaxy allowing us to identify any subjects that masses hosted in spiral galaxies at higher redshifts may have been previously misclassified. Once the (greater distance) if the correlation can be shown to spiral galaxies are confirmed and deprojected, vol- hold at these large distances. Measuring the spiral unteers are then tasked with tracing over any visi- arm pitch angles may be more reliable than current ble arms. These tracings are input into an algorithm methods as pitch angle techniques are dependent on called P2DFFT that is used to measure the degree of imaging rather than spectra. Although, it is currently unknown if measurement techniques applied to lo- winding of the arms (PA). Applying the MBH – PA relationship will allow us to identify any IMBH can- cal galaxies are also effective where the redshift is didates. These candidates are flagged for follow-up high and the resolution is lower. High redshift and spectroscopic observations which will be used to in- low resolution obviously makes the determination of the spiral arm pitch angle, at least, more diffi- dependently confirm their mass via the MBH – σ re- lationship. cult and prone to errors. We propose to continue our investigation of the selection biases and errors inherent in applying local galaxy measurement tech- 202.04 — A Comparison of Supermassive Black niques to high redshifted galaxies by working off of Hole Mass of NGC 4151 Using Different Methods our previously made progress, and attempting to de- Ismaeel Al-Baidhany1 tect redshifted spiral galaxy simulations as spirals 1 physics, Al-Mustansaryah University (Baghdad, Iraq) from survey data that they will be inserted into, mea- suring their spiral arm pitch angles, forming a se- Abstract We present a new estimate of the black hole lection bias matrix and measurement error matrix, (BH) mass in the Seyfert 1 galaxy, NGC 4151. We se- and then analyzing them for results. Both the selec- lected a sample of nearly face-on spiral galaxy and tion bias and measurement error matrix will be func- tions of pitch angle and other specified properties,

53 and will be made publicly available for the purpose 7 Siena College (Albany, New York, United States) of easily accessing data, applying correlations, and 8 Dartmouth College (Hanover, New Hampshire, United States) being referenced for other research. One thing we 9 NRAO (Charlottesville, Virginia, United States) will be able to use to our advantage when measur- 10 University of Kansas (Lawrence, Kansas, United States) ing spiral arm pitch angles is the relation predicted by density wave theory that the higher the concen- The circumgalactic medium (CGM) of galaxies holds tration of central mass in a galaxy the tighter their large, metal-enriched gas reservoirs. The origin of spiral arms (pitch angle) will be, and the lower the this gas remains elusive, but expulsion from galaxies concentration of central mass in a galaxy the looser through metal-enriched galactic winds plays a role. their spiral arms will be. We present a detection of an enormous, 100 kpc ion- ized gas nebula in [OII] with the Keck Cosmic Web 202.06 — Enhanced X-ray emission from candidate Imager (KCWI). It surrounds a compact star-forming Lyman continuum emitting galaxies galaxy at z ∼ 0.5. The hourglass shape of the nebula, high-velocity ionized and molecular outflows, and Jesse K. Bluem1; Philip Kaaret1; Andrea H. Prestwich2; young plus poststarburst stellar population are con- Matthew Brorby1 sistent with multiple gas ejection episodes over the 1 University of Iowa (Iowa city, Iowa, United States) past several hundred Myr. The nebula reaches well 2 Harvard-Smithsonian, CfA (Cambridge, Massachusetts, United beyond the galaxy’s stars and perhaps to a substan- States) tial fraction of the virial radius, thus connecting the galaxy to its CGM. The reionization of the early universe may have been helped by X-ray binaries. Feedback from X-ray bi- 202.08 — High Resolution Three-Dimensional naries may clear paths of low column density out of Hydrodynamic Relativistic Jet Simulations of galaxies, enabling the leakage of Lyman continuum Radio-Loud AGN radiation. However, the study of such distant galax- ies is not feasible, so we instead turn to local analogs. Nicholas Tusay1; Xuanyi Zhao1; Terance Schuh1; We studied the X-ray properties of 8 potential Ly- Nicholas Juliano1; Paul J. Wiita1 man leaking analog galaxies using Chandra obser- 1 Physics, The College of New Jersey (Pennington, New Jersey, vations. These galaxies were selected on the basis of United States) weak emission lines and a predominately blue color. These criteria favor low column densities and imply Jets emanating from radio-loud active galactic nu- the presence of young stars in the potential analogs. clei exhibit varying morphologies, which are usually X-ray luminosities were found for point sources iden- classified as either Fanaroff-Riley I (weaker sources tified in the galaxies, as well as for the full extent dominated by jets that have destabilizied) or FR II of the galaxies. Three of the galaxies have X-ray lu- (strong sources with jets that remain stable and ter- minosities well above theoretical calculations based minate in hot spots). We use the Athena relativis- on metallicity and star formation rate. These results tic hydrodynamics code to model the propagation of support the concept that the presence of X-ray bina- such jets in three dimensions. The critical initial pa- ries may have been important to the process of reion- rameters are the jet velocity and ratio of jet density ization. to that of the ambient medium, which determine the jet power and determine the type of radio galaxy that 202.07 — A 100 kpc Ionized Gas Outflow develops. We previously computed a suite of simu- Connecting a Compact Galaxy to its lations with a wide array of these parameters at a rea- Circumgalactic Medium sonably high resolution and characterized the types of jets that developed. With additional computa- David Rupke1; Alison L. Coil2; Gene Leung2; James tional power now available, we have now improved Geach4; Christina A. Tremonti3; Ryan C. Hickox7; the resolution of many of these simulations by in- Amanda A. Kepley8; John Moustakas6; Paul Sell5; Alek- creasing the number of zones per jet radius from 10 to sandar Diamond-Stanic10; Gregory Rudnick9 20. For a selection of inlet jet velocities and densities 1 Rhodes College (Memphis, Tennessee, United States) we compare these higher resolution simulations to 2 Bates College (Lewiston, Maine, United States) the previous runs to better analyze the distinguish- 3 UCSD (La Jolla, California, United States) ing characteristics of these propagating jets, such as 4 University of Wisconsin (Madison, Wisconsin, United States) turbulence within the cocoon and shock structures 5 University of Hertfordshire (Hertfordshire, United Kingdom) within the jet column. These allow us to more con- 6 University of Crete (Heraklion, Greece)

54 fidently classify each jet and refine the boundary be- 202.10 — Modelling Narrow NV z(abs)∼z(em) tween the FR I and FR II classes. Absorbers in the HST/COS Spectra of Radio-selected Quasars 202.09 — Toward a More Physical, Self-consistent Lacie Gladding1; Hayden Ruff1; Rajib Ganguly1; Model of Narrow z(abs)∼z(em) Absorbers in Alexandria Bakhsh1; Cordell Harris1 Quasar Spectra 1 University of Michigan - Flint (Flint, Michigan, United States) Alexandria Bakhsh1; Cordell Harris1; Rajib Ganguly1; Lacie Gladding1; Hayden Ruff1 From studies of high-resolution ultraviolet spectra 1 University of Michigan-Flint (Flint, Michigan, United States) (e.g., Misawa et al. 2007, Ganguly et al. 2013, Culli- ton et al. 2019a), it has become clear that absorption It is well-accepted that quasars are powered by the from the NV λλ1238.821, 1242.804 doublet yields accretion of matter onto supermassive black holes. purer samples of absorbers intrinsic to the quasar The accretion process appears to yield a variety of environment than their more common kin selected structures including a disk, a hot corona, broad and from CIV or OVI. A study of intrinsic NV absorbers narrow emission line regions, a jet, an obscuring with HST/COS spectra (Culliton et al. 2019b) re- torus, and a mass outflow. The mass outflow isof- vealed that NV absorbers observed in the spectra of ten regarded as the origin of not only the optical and radio-selected quasars occur in a variety of orienta- ultraviolet broad emission lines, but also provides a tions as gauged by the radio core fraction, which is natural explanation for ultraviolet broad absorption defined as the fraction of the radio emission aris- lines. The case of narrow absorbers (Δv <500 km/s) ing from the radio core relative to the total (core appearing on top of the broad emission lines is still plus lobes). Furthermore, the orientations in which outstanding in terms of origin and structure. Part of NV absorption is observed do not appear to be seg- the confusion is that narrow absorbers, commonly regated from the orientations where it is not ob- found with UV doublets from MgII, CIV, or OVI, served. A segregation would be expected from an arise from an eclectic variety of structures like inter- origin in a laminar flow. This is more consistent with stellar, intergalactic, and intragalactic gas. Recently, the absorbers arising from a clumpy medium sur- we have begun using the NV λλ1238.821, 1242.804 rounding the quasar . Here, we ap- doublet as these appear to preferentially select gas of ply a model from our companion effort (Bakhsh et an intrinsic origin. Here, we present a new approach al., these proceedings) to examine further the inher- to modelling NV absorbers from a more physical per- ent cloud structures that give rise to the observed spective than the standard modelling efforts (e.g., kinematic absorption profiles. From our preliminary partial covering of a plane-parallel slab in front of a analysis, we are able to show that it is unlikely that uniform background). Our goal is to have a utility the absorbing clouds are arranged in a spherically that is less computationally expensive than a detailed isotropic distribution as would be expected from an hydrodynamic simulation. Our new model incorpo- in situ origin at large distances from the central en- rates changes in the density of the absorbing struc- gine. Additionally, our modelling efforts may pro- tures (akin to inhomogeneous absorbers) and also vide preliminary estimates of the ionization condi- gradients in the background continuum source (the tions, as well as locations of the absorbers relative to accretion disk). For the disk, we currently employ the emission line gas. From these, we hope to better a Novikov-Thorne solution for a geometrically thin disentangle how the clumpy NV-bearing gas is dis- disk around a spinning black hole. Hence, we pa- tributed relative to the central engine of the quasar. rameterize the continuum using the black hole mass and spin, and the accretion rate. In addition, we an- 202.11 — The Evolution of Intermediate-Velocity ticipate adding a wind solution, and hot corona in Clouds on a Collision Course with the Galactic order to reproduce the broad emission lines. From Midplane this, we can entertain the projected locations of the 1 1 1 absorbers relative to the broad emission lines. The Matt Parker ; Robin L. Shelton ; Jason Galyardt ; Yasuo Fukui2; Kengo Tachihara2 potential inclusion of a jet may also increase the ap- 1 plicability of this model to radio-loud quasars. Physics and Astronomy, University of Georgia (Lavonia, Georgia, United States) 2 Nagoya University (Nagoya, Japan)

Many intermediate-velocity clouds (IVCs) appear to be falling toward the Milky Way’s disk, as evidenced

55 by their negative line of sight velocities and their 202.13 — Resolved observations of neutral cometary morphologies. We have simulated IVCs in hydrogen in nine z ∼ 0 luminous compact blue order to investigate the way in which they are trans- galaxies formed during their interactions with the interstel- 1 2,3 lar medium. Here, we present our simulations of Katie Rabidoux ; Daniel J. Pisano ; Catherine A. Garland4; Rafael Guzman5; Francisco Javier Castander6 one such cloud, IVC 86-36. We compare our simu- 1 lational results with the HI 21 cm emission observa- University of Wisconsin-Platteville (Platteville, Wisconsin, United States) tions made by Fukui et al. 2018, and we make predic- 2 tions about the cloud’s future behavior as it comes West Virginia University (Morgantown, West Virginia, United nearer to the galactic disk. States) 3 Green Bank Observatory (Green Bank, West Virginia, United States) 202.12 — Understanding the Relationship 4 Uncommon Charter High School (Brooklyn, New York, United Between the Circumgalactic Medium and the States) Interstellar Medium 5 University of Florida (Gainesville, Florida, United States) Martin Abram Flores1; Christopher M. Dupuis1; San- 6 Institut de Ciencies de l’Espai (Barcelona, Spain) chayeeta Borthakur1; Timothy M. Heckman2; Jason Tumlinson3 While bright, blue, compact galaxies are common at 1 Department of Physics, Arizona State University (Phoenix, Ari- z ∼ 1, they are relatively rare in the local universe, zona, United States) and their evolutionary paths are uncertain. We have 2 Johns Hopkins University (Baltimore, Maryland, United States) obtained resolved H I observations of nine z ∼ 0 lu- 3 Space Telescope Science Institute (Baltimore, Maryland, United minous compact blue galaxies (LCBGs) using the Gi- States) ant Metrewave Radio Telescope and Very Large Ar- ray in order to measure their kinematic and dynami- The circumgalactic medium (CGM) is the region ex- cal properties and better constrain their evolutionary tending from the disk of the galaxy to the virial ra- possibilities. We find that the LCBGs in our sample dius. As gas from the intergalactic medium (IGM) are rotating galaxies that tend to have nearby com- undergoes accretion, it has to flow through the CGM panions, relatively high central velocity dispersions, before it reaches the interstellar medium (ISM). The and can have disturbed velocity fields. We com- influence that the CGM has on the evolution of galax- pare our measurements to those previously made ies is still not fully understood. Previous studies on with single dishes and find that single-dish measure- L* galaxies provide evidence that CGM gas accretion ments tend to overestimate LCBGs’ rotation veloci- feeds the neutral gas content in the ISM. A similar ties and H I masses. We also find that LCBGs are study has not yet been conducted to show if these re- strongly rotationally supported at large radii, similar sults hold for lower mass galaxies, which are much to other disk galaxies, though within their half-light more abundant. We present the results of a dwarf radii the Vrot/σ values of their H I are comparable to galaxy survey investigating the connection between stellar Vrot/σ values of dwarf elliptical galaxies. The the neutral gas properties in the CGM and ISM. We disks of the LCBGs in our sample are gravitationally use 21 cm emission to probe the ISM and explore its stable, though conditions may be conducive to local relationship to the CGM by comparing it to Lyman gravitational instabilities at the largest radii. Such in- α (Lyα) absorption measurements obtained from the stabilities could lead to the formation of star-forming COS-Dwarfs program. We find that galaxies show a gas clumps in the disk, resulting eventually in a small good Lyα covering fraction in the inner CGM. How- central bulge or bar. ever, we find gaps in the neutral gas envelope inthe outer CGM of these galaxies. We do not find a cor- 202.14 — Tracing Young Stars in the Outer Disks relation between the strength of Lyα in the CGM of HI-rich Galaxy and HI content in the ISM, which was seen for Milky Mansi Padave1; Sanchayeeta Borthakur1; Rolf A. Way-like galaxies. As a result, we believe that there 1 2 1 are gaps in the CGM of dwarf galaxies due to loss of Jansen ; David A. Thilker ; Hansung Gim ; Robert Kennicutt3,4; Timothy M. Heckman2 circumgalactic gas via feedback owing to the lower 1 halo masses. School of Earth and Space Exploration, Arizona State University (Tempe, Arizona, United States) 2 Johns Hopkins University (Baltimore, Maryland, United States) 3 University of Arizona (Tucson, Arizona, United States) 4 Texas A&M University (College Station, Texas, United States)

56 We present the first results from the UV-DISK pro- empirical precision of σ = 0.60%, we conclude that 퐻0 gram aimed to trace recent star formation (≤100 the distance ladder measurement is not affected by Myrs) in the outer low-density regions of 35 low- local density contrasts, in agreement with cosmic redshift galaxies. These galaxies are HI-rich with HI variance of σ = 0.42% predicted from simulations 퐻0 disks that extend to twice the optical size, and have of large-scale structure. Given that uncertainty in the been probed via COS-QSO absorption spectroscopy distance ladder value is σ = 2.2%, this does not af- 퐻0 at impact parameter ρ ≤ 3R퐻퐼. We perform surface fect the Hubble tension. We derive a 5 σ constraint on photometry on GALEX UV and PanSTARRs g, r, i ob- local density contrasts on scales larger than 69 mega- servations for the sample, and combine it with VLA h−1 of δ < 27%. The presence of local structure HI-21 cm maps to investigate the physics of star for- does not appear to impede the possibility of measur- mation in the low-density outer disks of these galax- ing the Hubble constant to 1% precision. ies. Here, we present the scaling relations between the spatial extent of young stars (≤100 Myrs) in the 203.02 — Towards cosmology from Lyman-α galaxy disk and the HI disk. In particular, we discuss intensity mapping in HETDEX the Extended-UV disk of NGC 3344 which we have 1 also imaged in Hα. Combining HST COS-absorption Shun Saito 1 spectroscopy, VLA HI-21 cm imaging, UV and Hα Physics, Missouri University of Science and Technology (Rolla, photometry allows us to correlate the formation of Missouri, United States) young stars to the local ISM conditions and CGM properties and map the full transport route of gas Future galaxy redshift surveys generally plan to ob- from the CGM to the star forming disk serve emission lines from star-forming galaxies to measure the three-dimensional galaxy clustering. One ongoing example is the Hobby-Eberly Telescope 203 — Cosmology and Related Dark Energy Experiment (HETDEX). HETDEX is designed to observe one million Lyman-α emitters Topics Poster Session (LAEs) over 1.9 < z < 3.5 in a unbiased way using the Integral Field Unit. However, such a unbiased nature 203.01 — The Local Perspective on the Hubble of the HETDEX survey gives us an excellent oppor- Tension: Local Structure Does Not Impact tunity. Namely, every 3D pixel in principle encodes Measurement of the Hubble Constant the intensity of diffuse Lyman-α photons if exist. In W. D’Arcy Kenworthy1; Dan Scolnic3; Adam G. Riess1,2 this presentation, we discuss the feasibility of this so- 1 Johns Hopkins University (Baltimore, Maryland, United States) called Lyman-α intensity mapping as a cosmologi- 2 Space Telescope Science Institute (Baltimore, Maryland, United cal probe. We also introduce our simulation efforts States) in which the radiative transfer of Lyman-α photons 3 Duke University (Durham, North Carolina, United States) are post processed in the Illustris simulation in or- der to have better understanding of the distribution We use the largest sample to date of spectroscopic of Lyman-α photons in the Universe. SN Ia distances and redshifts to look for evidence in the Hubble diagram of large scale outflows caused 203.03 — Galaxies in Place of Quasars: Discovery by local voids suggested to exist at z<0.15. Our sam- of a Low Redshift Damped Lyman-α system in the ple combines data from the Pantheon sample with Spectrum of a Star Forming Galaxy the Foundation survey and the most recent release of 1 1 lightcurves from the Carnegie Supernova Project to Christopher M. Dupuis ; Sanchayeeta Borthakur ; Rachael Alexandroff2; Timothy M. Heckman3 create a sample of 1295 SNe over a redshift range of 1 0.01 20%, where the online in the following decade, a new method for density contrast δ = Δ ρ /ρ) proposed in some galaxy discovering intervening gas clouds at high redshifts count studies, and find no evidence of a change in will soon become possible. This method consists of the Hubble constant corresponding to a void with a using spectra of star forming galaxies, in place of sharp edge in the redshift range 0.023

57 quasars (QSOs), to search for intervening clouds. Al- to compare the observations with the predicted tem- lowing for this method are new ground-based tele- perature dependent ionization fractions. We utilize scopes that will have the sensitivity needed to ob- individual galaxy spectra in an effort to characterize tain high quality spectra of high redshift galaxies. the O VI absorption as being due to the IGrM and By using this method, we will dramatically increase not from the circumgalactic medium (CGM) of star the number of sightlines probed which are currently forming galaxies (Tumlinson et al. 2011). limited by the number of QSOs. As a proof of con- cept, we present the discovery of a damped Lyman- 203.05 — Automated Physics-Based Detection and α system (DLA) in the spectrum of a low redshift Identification of Intergalactic Clouds using (z=0.175) star forming galaxy using data obtained Probabilistic Programming from HST. This DLA is associated with the circum- 1 1 galactic medium (CGM) of a foreground galaxy at Rashmeet Kaur Nayyar ; Mansi Padave ; Sanchayeeta 1 1 z=0.17 probed at an impact parameter of 43 kpc. We Borthakur ; Siddharth Srivastava 1 detect H I at N(HI)=3x1020 cm−2, along with multi- Arizona State University (Tempe, Arizona, United States) ple low-ionization transitions such as C II, Si II, and Si III in the spectrum of the DLA. This is a rare dis- Absorption lines in the spectra of distant Quasi- covery as, to the level capable of current instruments, stellar objects are our main source of information most QSO sightlines have been probed. With the im- about physical conditions and composition of mat- proved sensitivity of new 30-meter class telescopes ter in the intergalactic medium. However, manual such as the Giant Magellan Telescope and the Ex- analysis of such spectra is time-consuming and error- tremely Large Telescope, it will be possible to probe prone, in part due to the unknown redshifts of ab- intervening gas and CGMs at high redshifts using sorption lines and the unknown number of interven- this method. ing clouds. Automatic analysis has also been chal- lenging for this problem: observational uncertain- ties make it difficult to use combinatorial search tech- 203.04 — Characterizing the Dark Matter Halos of niques, and approaches based on probabilistic infer- Galaxy Groups and Their Hidden Baryonic ence typically require prior knowledge of the num- Content ber of clouds. We present a new approach that sup- Tyler McCabe1; Sanchayeeta Borthakur1; Timothy M. ports a variety of QSO spectra studies while account- Heckman2; Jason Tumlinson3; Gerard Mark Voit4 ing for observational uncertainties as well as the un- 1 School of Earth and Space Exploration, Arizona State University known numbers and types of intervening clouds. We (Tempe, Arizona, United States) use a probabilistic programming language, Bayesian 2 Johns Hopkins University (Baltimore, Maryland, United States) Logic (BLOG), that extends first-order logic seman- 3 Space Telescope Science Institute (Baltimore, Maryland, United tics with probability theory and allows efficient spec- States) ifications for physics-based probabilistic models. We 4 Michigan State University (East Lansing, Michigan, United show how our system would utilize the equivalent States) width and position of absorption lines in the spec- tra as observations. It also provides a rich query lan- A large fraction of galaxies today reside in groups guage for investigating properties of the possible in- and the dominant form of baryons in these groups is tervening clouds. Answers to the resulting queries predicted to be a diffuse Intragroup medium (IGrM). would be consistent with (and supported by) the in- Despite its importance, direct observational detec- put physics models. We will evaluate this repre- tion of the IGrM has been limited to the most mas- sentational approach using techniques for approx- sive groups where the IGrM is hot enough to emit imate probabilistic inference on the Hubble Space soft X-rays. Therefore, we have mounted a controlled Telescope (HST) COS data that cover a range of back- absorption-line experiment to search for the IGrM ground QSO up to Z = 1. The flexibility and ro- using a pre-defined sample of groups. The COS- bustness of this analytical approach would be invalu- IGrM survey is a medium-sized Hubble Space Tele- able in evaluating scientific hypotheses with large scope (HST) program to map the IGrM of 19 low-z datasets such as those from HST as well as with data (0.08 < z < 0.17) galaxy groups with the Cosmic Ori- expected from forthcoming large observatories such gins Spectrograph (COS). Using these data, Lyman as GMT, ELT, and TMT. α, O VI, and other absorption lines were measured to determine the column density of the intragroup gas. Collisional ionization equilibrium models were used

58 203.06 — Cosmic Voids as Laboratories for studies via thermotes (Feria, AAS 230). Thermotes Neutrino Physics surfaced in LTT in 2014 from the derivation of

1 1 2,3 the entropy of flexible-phase mediums for use in Christina Kreisch ; Alice Pisani ; Carmelita Carbone ; lifespan studies. They simplify entropy finding Jia Liu1; Adam Hawkin4; Elena Massara5; David N. 1,5 5,6 and their energy is eTh=NDoFkBT/2 where kB is the Spergel ; Benjamin Wandelt , T is the temperature of the 1 Princeton University (Princeton, New Jersey, United States) 2 medium and NDoF is the number of degrees of Università degli studi di Milano-Dipartimento di Fisica (Milano, freedom (DoF) for a particle, e.g., 3 for photon-gas Italy) 3 (PG) photons and 2 for black-hole (BH) particles in INAF-Osservatorio Astronomico di Brera (Milano, Italy) its event horizon. For the BH and PG their entropy 4 Aix-Marseille Université (Marseille, France) 5 is kB/2 times the ratio of their mass-energy over Center for Computational Astrophysics, Flatiron Institute (New the thermote energy, which then via the 2nd law of York City, New York, United States) 6 thermodynamics leads to the LTT conjecture that Institut d’Astrophysique de Paris (Paris, France) T decreases with time with the thermote energy loss fueling the Universe’s expansion. Moreover, Massive neutrinos uniquely affect cosmic voids. We the eV mass of the BH and PG thermotes at the explore their impact on void clustering using both cosmic microwave background (CMB) temperature the DEMNUni and MassiveNuS simulations. For of 2.725 is found to be 235.14 μeV and 352.71 voids, neutrino effects depend on the tracers. As μeV, respectively, values which fall within the 50 neutrino mass increases, the number of small voids to 1,500 μeV range for the axion, a top dark matter traced by cold dark matter particles increases and candidate (Borsanyi, et al. 2016, Nature). In LTT the number of large voids decreases. Surprisingly, the shape of the medium of mass M and volume when massive halos are used as tracers, we see the V is modeled as a sphere of radius r where at its opposite effect. How neutrinos impact the scale at center its point-mass resides. In this LTT model which voids cluster and the void correlation is sim- there are M/m gyrador particles whose total kinetic ilarly sensitive to the tracers. This scale dependent G energy matches the gravitational bias is not due to simulation volume or halo density. GM2/2r of the medium. Each gyrador of mass m We also present new results on scaling relations be- G orbits a quantum of operation (QoO) mass 훿M at the tween tracers and voids as well as the impact of neu- center of a sphere of radius 훿r with orbiting-speed trino mass on void bias. The interplay of these sig- v=(G훿M/훿r)1/2 and 훿M/훿r=M/r. In LTT the kinetic natures in the void abundance, clustering, and bias energy m v2/2 of the gyrador is set equal to the leaves a distinct fingerprint that could be detected G thermote energy e which then yields m =2re /GM with upcoming observations and help break degen- Th G Th whose evaluation for the sun and humans matches eracies between different cosmological parameters. the average mass of sun particles and human cells. This work paves the way to exploit cosmic voids in DESI, PFS, Euclid, and WFIRST to constrain the mass of neutrinos. 203.08 — ΛCDM or self-interacting neutrinos? - how CMB data can tell the two models apart 203.07 — First Principles of Linger-Thermo Minsu Park1; Christina Kreisch1; Jo Dunkley1; Boryana Theory, a Time-Complementary Duality in Hadzhiyska2; Francis-Yan Cyr-Racine2,3 Physics, Inherently Lead to Average Mass of Star 1 Physics, Princeton University (Princeton, New Jersey, United Particles and Organism Cells States) 2 Harvard University (Boston, Massachusetts, United States) Erlan H. Feria1 3 University of New Mexico (Albuquerque, California, United 1 CUNY College of Staten Island, Department of Engineering and States) Environmental Science (Staten Island, New York, United States) Of the many proposed extensions to the Lamb- Linger-thermo theory (LTT) is part of a time- daCDM paradigm, a model in which neutrinos self- complementary past-uncertainty/future-certainty interact until close to the epoch of matter-radiation spacetime duality in physics with uncertainty equality has been shown to provide a good fit to initial state that yields maximally efficient and current cosmic microwave background (CMB) data, affordable solutions such as in radar (Feria, 2014 while at the same time alleviating tensions with late- SPIE Newsroom article 10.1117/2.1201407.005429 time measurements of the expansion rate and mat- & 2018 US Patent 10,101,445). LTT has been used ter fluctuation amplitude. Interestingly, CMB fits to in astrobiology (Feria, AAS 49 PS) and dark-matter this model either pick out a specific large value of the

59 neutrino interaction strength, or are consistent with The challenges of dealing with the upcoming data the extremely weak neutrino interaction found in from the the Daniel K. Inoue Solar Telescope (DKIST) LambdaCDM, resulting in a bimodal posterior dis- are diverse. DKIST will easily dwarf even the data tribution for the neutrino self-interacting cross sec- volumes created by SDO, but when you add in the tion. In this paper, we explore why current cos- longevity of the observatory (two full solar cycles), mological data select this particular large neutrino the complexity of the 5 instrument packages on the self-interaction strength, and by consequence, disfa- Coude platform, the desire to create an automated vor intermediate values of the self-interaction cross calibration pipeline, designed to remove the instru- section. We show how it is the l ≥1000 cosmic mi- ment effects of a ground based teelscope for all obser- crowave background temperature anisotropies, most vation sets, and the need to be able to distribute the recently measured by the Planck satellite, that pro- large datasets in an effecient, reliable manner, then duce this bimodality. We also establish that smaller the true scale of the tasks become obvious. Here I scale temperature data, and improved polarization discuss how we meet all these challenges, leveraging data measuring the temperature-polarization cross- not only best in breed open source source software, correlation, will best constrain the neutrino self- but also engineering design, building and testing interaction strength. We forecast that the upcom- principles, to create a next generation solar physics ing Simons Observatory should be capable of distin- data center capable of meeting the challenges DKIST guishing between the models. presents.

204.03 — Localized Quasi-Periodic Fluctuations in 204 — Solar Physics Division C II, Si IV, and Fe XXI Emission During (SPD), Poster Session II Chromospheric Evaporation in a Flare Ribbon Observed by IRIS and RHESSI on 2017 September 204.01 — DKIST User Tools for Level 1 Data 9 Stuart Mumford1; Fraser Watson2; Alisdair R. Davey2 Jeffrey W. Brosius1; Andrew Inglis1 1 1 University of Sheffield (Holmfirth, United Kingdom) Catholic University of America (Greenbelt, Maryland, United 2 NSO (Boulder, Colorado, United States) States)

The DKIST user tools aim to lower the barrier of en- We investigate the onset of a GOES M3.7 flare on try to scientific discovery with the DKIST level one 2017 September 9 with rapid cadence (9.4 s) ultravi- data. The tools provide standard python interfaces to olet stare spectra obtained with IRIS in five 1-arcsec the data and coordinate information in a way that en- slit segments. Our analysis is based primarily on in- ables interoperability with the wider Python ecosys- tegrated intensities and Doppler velocities of C II at tem. The user tools are based on widely used Python 1334.5 Angstroms (T ∼ 0.025 MK), Si IV 1402.7 (0.079 packages such as Dask and matplotlib as well as the MK), and Fe XXI 1354.1 (11 MK). The four segments SunPy and Astropy packages. The DKIST user tools within the ribbon show systematically earlier start- will provide Python interfaces for: ing times for the low-T lines (C II and Si IV) than Searching the DKIST Data Centre, retrieving meta- Fe XXI; further, the velocities derived for Fe XXI are data about datasets in ASDF format and download- generally directed upward along the line of sight. ing whole datasets or subsets as collections of FITS This is consistent with the standard flare model, in files. Maintaining a record of retrieved datasets and which beams of nonthermal particles ionize and heat their locations. Loading data from large numbers the chromosphere, and drive chromospheric evap- of FITS files efficiently and transparently Performing oration: as the temperature and ionization stages high-level operations on the data and coordinate in- of the chromospheric plasma increase, intensities of formation in tandem. emission lines also increase, first from lines in lower This poster will provide demonstrations of imple- stages of ionization, and later from lines in higher mented and future functionality and discuss the in- stages of ionization. Where quasi-periodic fluctua- tegration with analysis and visualization libraries. tions were observed in the ribbon in both low-T and Fe XXI emission, the peaks in the low-T light curves 204.02 — The DKIST Data Center - Curating, preceded those in the Fe XXI light curve, and peaks Calibrating and Distributing DKIST Data in the Fe XXI upward velocity typically also preceded those in the Fe XXI light curve. Thus the behavior of 1 Alisdair R. Davey each individual fluctuation was similar to that ofa 1 National Solar Observatory (Boulder, Colorado, United States)

60 standard flare, suggesting that each individual fluc- associated with coronal mass ejections (CMEs) when tuation was due to a separate injection of nonthermal a filament embedded under the fan dome erupts. particles into the chromosphere. Based on RHESSI Here we study the M8.7 CRF occurred in NOAA AR HXR observations, we estimate sufficient beam en- 12242 (SOL2014-12-17T04:51), which is accompanied ergy flux to drive explosive chromospheric evapora- by a CME but the active region filaments remain in- tion. tact. Using coronal magnetic field reconstructed un- der the nonlinear force-free field assumption, we find 204.04 — Hard X-ray Spectroscopy of Six NuSTAR that the outer spine-like loops form a twisted mag- Microflares netic flux rope (MFR1) rooted at the edge of the fan- dome field with opposite twist, and that there isa 1 1 Jessie McBrayer Duncan ; Lindsay Glesener ; Iain second flux rope (MFR2) lying above the main polar- 2 3 4 Hannah ; David M. Smith ; Sam Krucker ; Hugh S. ity inversion line (PIL). We divide the event evolution 2 5 Hudson ; Brian Grefenstette into two main stages based on EUV observations. (1) 1 Physics and Astronomy, University of Minnesota (Minneapolis, The event onset is featured with small bidirectional Minnesota, United States) jetting activities between the sheared filament field 2 University of Glasgow (Glasgow, United Kingdom) and MFR1, immediately followed by an upward mo- 3 University of California, Santa Cruz (Santa Cruz, California, tion of MFR1. During this first stage, the inner/outer United States) and the circular ribbons begin to brighten up. (2) Af- 4 University of California, Berkeley (Berkeley, California, United ter about 10 minutes, another ejection stems from the States) main PIL region. This is most probably related to an 5 California Institute of Technology (Pasadena, California, United eruption of MFR2, as the twist of MFR2 footpoints States) exhibits a clear decrease subsequently. In this second stage, all ribbons are significantly enhanced. We dis- Hard X-ray (HXR) emission in solar flares can orig- cuss these results in favor of a scenario where the ini- inate from regions of high temperature plasma, as tial reconnection between the sheared filament field well as from non-thermal particle populations. Both and MFR1 triggers the latter to erupt, then the erupt- of these sources of HXR radiation make solar obser- ing MFR1 interacts with the overlying fan-like field vation in this band important for study of flare en- to allow a second eruption of MFR2. This event thus ergetics. NuSTAR is the first HXR telescope with represents a new type of eruptive CRFs caused by an direct focusing optics, giving it a dramatic increase unstable outer spine-like loops without involving a in sensitivity over previous indirect imaging meth- filament. ods. Here we present NuSTAR observation of six microflares from one solar active region during a 204.06 — Analyzing deviations from optically thin period of several hours on May 29th, 2018. Spec- emission in flare ribbon plasma using IRIS tral fitting of emission at each flare time shows ex- observations of Si IV resonance lines cess high energy emission over an isothermal spec- tral component in all six flares. The most likely ori- Sean Brannon1; Charles Kankelborg1 gin of this excess could be either additional volumes 1 Montana State University (Bozeman, Montana, United States) of high-temperature plasma, or non-thermally accel- erated particles. For each event, characterization of It is well-established that the Si IV resonance line pair this excess is presented, including determination of at 1394 and 1403 Å observed by the Interface Region upper limits on the non-thermal emission possible in Imaging Spectrograph (IRIS) exhibits a 2:1 intensity events where it is not directly observed. ratio in optically thin plasma. Deviations from this ratio may arise from optical thickness (Mathioudakis 204.05 — The Eruption of Outer Spine-like Loops et al. 1999) and/or geometric effects (Kerr et al. 2005) Leading to a Double-Stage Circular-Ribbon Flare in the emitting plasma. These effects are expected to be particularly prevalent in the dense chromospheric 1 1 1 Chang Liu ; Jeongwoo Lee ; Haimin Wang plasma that forms the ribbons during a flare, and the 1 New Jersey Institute of Technology (Newark, New Jersey, United Si IV resonance line ratio therefore provides a diag- States) nostic of the plasma conditions at the flare loop foot- points. Recently, Kerr et al. (2019) used RADYN sim- Studying circular-ribbon flares (CRFs) and the re- ulations to demonstrate that a significant fraction of lated magnetic structure/topology can advance our the Si IV flare ribbon emission may form at cooler knowledge of solar eruptions in general. Although temperatures, even for relatively small flares. Their they are usually confined events, CRFs can also be

61 results showed changes to both line shape and inten- 204.08 — Statistical Study of Solar Flares sity in flare plasma, and they recommended caution Observed in Lyman-α Emission During Solar when interpreting Si IV emission in flare ribbons. Cycle 24 Using GOES-15

Additionally, they noted that only a handful of stud- 1,2 ies using IRIS observations have reported the line ra- Ryan O. Milligan 1 University of Glasgow (Glasgow, United Kingdom) tio in flares. In this work, we report on our workto 2 create a catalog of the line ratio for additional flare NASA Goddard Space Flight Center (Greenbelt, Maryland, ribbon events in the IRIS observation database. We United States) select IRIS observations of flares that record both Si The chromospheric Lyman-α line of hydrogen (Lya; IV resonance lines with an 8-step or fewer raster, and 1216A) is the strongest emission line in the so- identify 28 candidate observations for which the flare lar spectrum. Fluctuations in Lya are known to ribbon is covered by the spectrograph slit. We estab- drive changes in the D-layer of Earth’s ionosphere lish criteria for identifying spectra that capture flare (>70km), and recent studies suggest that during solar ribbon emission and for eliminating spectra that con- flares, up to 10% of the energy deposited in the chro- tain defects (e.g. saturated pixels). We calculate line mosphere by nonthermal electrons is radiated away intensities (less background contribution) and con- by the Lya line alone. Despite the energetic impor- struct the line ratio for all selected spectra in each tance of Lya there have been relatively few studies in observation, and report the mean, median, and devi- the literature that focus on the behaviour of Lya emis- ation of the line ratio for each flare ribbon. Based on sion during flares. This work presents a statistical our results, we briefly discuss physical implications study of almost 500 M- and X-class flares observed for interpreting Si IV emission in flare ribbons. in Lya emission by the EUVS instrument on GOES- 15 during Solar Cycle 24. It was found that up to 100 204.07 — Multi-instrument Comparative Study of times more energy can be radiated by Lya compared Temperature, Number Density and Emission to soft X-rays (also a driver of D-layer fluctuations); Measure during the Precursor Phase of a Solar that Lya enhancements during flares are comparable Flare to or greater than those measured due to solar ro- Nian Liu1; Ju Jing1; Haimin Wang1; Yan Xu1; Mark tation variability, albeit on much shorter timescales; Cheung2; G.D Fleishman1 and that center-to-limb variations appear to be neg- 1 Applied Physics, New Jersey Institute of Technology (East ligible despite Lya being optically thick. Newark, New Jersey, United States) 2 Lockheed Martin Solar and Astro Laboratory (Palo Alto, Califor- 204.09 — Modeling of Electron Acceleration and nia, United States) Transport along Realistic Magnetic Loops Yihong Wu1,2; Alexis Paul Rouillard1,3; Athanasios The precursor brightenings of solar flares hold valu- 1,2 4 4 able clues concerning the flare triggering and energy Kouloumvakos ; Rami Vainio ; Alexandr Afanasiev ; Illya Plotnikov1 release mechanisms, but have not been well stud- 1 ied. This paper presents a multi-instrument study Institut de Recherche en Astrophysique et Planétologie (Toulouse, of the two precursor brightenings prior to the M6.5 Haute-Garonne, France) 2 Université de Toulouse III (Toulouse, France) flare (SOL2015-06-22T18:23) in NOAA active region 3 12371, with a focus on the temperature (T), number Centre National de la Recherche Scientifique, UMR 5277 (Toulouse, France) density (n) and emission measure (EM) of these two 4 precursors. The multi-instrument data used in this University of Turku (Turku, Finland) study were obtained from four instruments with va- We provide an explanation on the origin of the ob- riety of wavelengths, i.e., the Solar Dynamics Obser- served solar hard X rays during the 1 September vatory’s Atmospheric Imaging Assembly (AIA) in six 2014 solar eruptive event. The CME-driven coronal EUV passbands, the Expanded Owens Valley Solar shock is magnetically connected to the visible disk, Array (EOVSA) in microwave, RHESSI in hard X-ray suggesting the coronal shock may be the strongest and GOES in soft X-ray. We compare the tempo- candidate as the particle accelerator. A 3D triangu- ral variation of T, n and EM derived from different lation technique, based on remote-sensing observa- data sets during the precursor period and discuss the tions is used to model the expansion of the CME differences in terms of the sensitivity of the instru- shock. Realistic time-dependent evolution of shock ments. properties along field lines and realistic background

62 fields for particle transport from the shock to the so- 204.12 — FOXSI-2 Solar Microflares: Hard X-ray lar surface are obtained. We develop Shock-Drift Ac- Spectroscopy and Flare Energetics celeration and Diffusive-Shock Acceleration models 1 1 with multiple interactions due to particles bouncing Juliana Vievering ; Lindsay Glesener ; Subramania Athiray Panchapakesan1,5; Juan Camilo Buitrago- along magnetic loops. We look into the effect of mir- 2 3 1 4 ror force on transport process. The returning of the Casas ; Daniel Ryan ; Sophie Musset ; Andrew Inglis ; Steven Christe3; Sam Krucker2 downstream electrons to the upstream is also consid- 1 ered. We verify that electrons can be accelerated to University of Minnesota (Minneapolis, Minnesota, United States) 2 Space Sciences Laboratory (Berkeley, California, United States) a few MeV and reach the chromosphere producing 3 hard X-rays. NASA Goddard Space Flight Center (Greenbelt, Maryland, United States) We also study the type II radio bursts during this 4 event and provide an interpretation for the observa- The Catholic University of America (Washington, District of tional characteristics. Columbia, United States) 5 Marshall Space Flight Center (Huntsville, Alabama, United States) 204.10 — A Database of Flare Ribbon Properties From Solar Dynamics Observatory Sensitive measurements of solar flares in the hard X- Maria D. Kazachenko2,1 ray regime are necessary for investigating energy re- 1 UC Berkeley (Berkeley, California, United States) lease and transfer during flaring events, as hard X- 2 CU Boulder (Boulder, Colorado, United States) rays provide insight into the acceleration of electrons and emission of high-temperature plasmas. Due to We analyze a database of >3000 of solar flare ribbon use of indirect imaging, past solar-dedicated instru- events corresponding to every flare of GOES class ments in this energy range have been fundamen- C1.0 and greater within 45 degrees from the disk cen- tally limited in sensitivity and dynamic range. By ter, from April 2010 until April 2019, observed by the instead using a direct imaging technique, the struc- Solar Dynamics Observatory (SDO). For every event ture and evolution of even small flares and active re- in the database, we compare GOES X-ray flare prop- gions can be investigated in greater depth. The Fo- erties with corresponding active-region and flare- cusing Optics X-ray Solar Imager (FOXSI), a hard X- ribbon properties. We present the results and discuss ray instrument flown on three sounding rocket cam- other flare quantities one could derive from the SDO paigns, seeks to achieve these improved capabilities to deepen our understanding of solar flare physics. by using focusing optics for solar observations in the 4-20 keV range. During the second flight, which oc- 204.11 — On the observation of a classical curred on 2014 December 11, FOXSI-2 observed two loop-prominence system during the 2017 microflares, estimated as GOES class A0.1 and A0.3. September 10 flare. Here we present imaging and spectral analyses of these microflares, investigating the nature of energy Juan Carlos Martinez Oliveros1; Sam Krucker1; Juan release and exploring the structure and dynamics Camilo Guevara Gomez2 in comparison to larger flares. Through this work, 1 University of California Berkeley (Berkeley, California, United we find evidence for high-temperature plasma (∼10 States) MK) as well as spatial and temporal complexity for 2 University of Oslo (Oslo, Norway) microflares that are an order of magnitude fainter than those observed by previous solar-dedicated in- We report observations of white-light ejecta in the struments in this energy range, highlighting the ben- low corona after the 2017 September 10 flare, us- efits of direct imaging. ing data from the Helioseismic and Magnetic Imager (HMI) of the Solar Dynamics Observatory. We report 204.13 — Mg II NUV Spectra in Solar Flares: the observation of a classical loop-prominence sys- Modelling approaches and Velocity Diagnostics tem, but are brighter than expected and possibly seen here in the continuum rather than line emission. We Graham S. Kerr1; Joel C. Allred1; Mats Carlsson2 studied the spatial and temporal relation between 1 NASA/GSFC (Greenbelt, Maryland, United States) RHESSI X-ray and the white-light emissions. We also 2 University of Oslo (Oslo, Norway) studied the HMI spectroscopic data to determine the most probable emission mechanism that can explain The Interface Region Imaging Spectrograph (IRIS) the observation of the loop-prominence system. has observed the Mg II NUV spectrum (the h & k resonance and the subordinate triplet), in hundreds

63 of solar flares. These lines form throughout the where there are discrepancies between experiments chromosphere, offering excellent diagnostic poten- and theory. tial and a window into the location of flare energy deposition. A number of studies have attempted to 205.02 — Status & Needs of Astrophysical Plasma forward model both the general properties of these Models lines in flares, and specific flare observations. Gener- 1 1 ally, these investigations have post-processed snap- Randall K. Smith ; Adam Foster 1 shots of solar atmospheres from hydrodynamic or ra- Smithsonian Astrophysical Observatory (Cambridge, Mas- diation hydrodynamic flare simulations through ad- sachusetts, United States) vanced radiation transport codes. There has, how- ever, not been a survey of how the physics included X-ray emission from energetic astrophysical plasmas in these radiation transport codes affects the solu- is typically analyzed using a range of software pack- tion. We present here a detailed study showing what ages, including SPEX and XSPEC. Within these pack- physics must be included when forward modelling ages are several different models for different types these lines, including the use of partial redistribu- of astrophysical plasmas. The most complex involve tion (PRD), the specific treatment of (PRD), the need detailed modeling of spectral line emission from for a sufficiently large model atom, the inclusion thermal or photoionized plasma, based on the SPEX, of Mg I in NLTE, the inclusion of other species in AtomDB or XSTAR plasma codes. These plasma NLTE, and the impact of using non-equilibrium hy- codes combine atomic data with models of electron, drogen populations. Futher, we contrast Mg II com- photon or collision dominated plasmas to puted in statistical equilibrium with a computation produce a complete spectrum for a range of plasma that includes non-equilibrium effects. Finally, we ap- conditions, including temperature, density, elemen- ply commonly used observational metrics for infer- tal composition and more. While it could be ex- ring Doppler speeds to the synthetic spectra, demon- pected that these plasmas produce identical results strating that optical depth and radiation transfer ef- for the same input plasma conditions, there are sev- fects can confuse the interpretation of those measure- eral reasons why they do not, relating to different in- ments. put atomic data, model assumptions and model in- tentions. I will discuss the different plasma models, their applications, underlying assumptions, and the 205 — Laboratory Astrophysics similarities and differences in their results, as well as Division (LAD), Poster Session future needs for missions such as XRISM and Athena 205.03 — Relativistic Atomic Structure of the Au II 205.01 — Laboratory Calibrations of Fe XII-XIV Isoelectronic Sequence: opacity data for kilonova Line-Intensity Ratios for Electron Density ejecta Diagnostics Alicia Flowers1; Yier Wan1; Zahra Taghadomi1; P. Michael Hahn1; Thusitha Arthanayaka1; Peter Stancil1; Brendan McLaughlin2; S. Loch3; S. Bromley4; Beiersdorfer2; Gregory V. Brown2; Ming Gu3; Natalie J. P. Marler4; C. E. Sosolik4 Hell2; Tom Lockard2; Daniel Wolf Savin1 1 Department of Physics & Astronomy, University of Georgia 1 Columbia University (New York, New York, United States) (Athens, Georgia, United States) 2 Lawrence Livermore National Laboratory (Livermore, California, 2 Centre for Theoretical Atomic and Molecular Physics (CTA- United States) MOP), School of Mathematics and Physics, Queen’s University 3 Space Sciences Laboratory, University of California Berkeley (Belfast, United Kingdom) (Berkeley, California, United States) 3 Department of Physics, Auburn University (Auburn, Alabama, United States) We have used an electron beam ion trap to measure 4 electron-density-diagnostic line-intensity ratios for Clemson University (Clemson, South Carolina, United States) extreme ultraviolet lines from Fe XII, XIII, and XIV On August 17, 2017, the Laser Interferometer Grav- at wavelengths of 185-205 and 255-276 Angstrom. itational Wave Observatory (LIGO) and VIRGO de- These ratios can be used as density diagnostics for tected gravitational waves (GW170817) propagating astrophysical spectra and are especially relevant to from a binary neutron star merger, in which ejected solar physics. We have compared our results to material from the merger emitted thermal radiation atomic calculations using the Flexible Atomic Code in the optical and near-infrared (NIR). The ejecta is and identified some lines that are reliable and others classified into two classes based on the atomic weight

64 of the chemical composition: the first class is com- situ diagnostic tools, used for the detection and char- posed primarily of light (atomic mass number < 140), acterization of the species present in the expansion: and the second class is composed of heavy elements a Cavity Ring Down Spectroscopy (CRDS) and fluo- (atomic mass number > 140). The latter incites the rescence spectroscopy systems operating in the UV- possibility that highly-dense mergers are the cre- Visible range [2], and a Reflectron Time-Of-Flight ation sites for heavier elements, as they are created Mass Spectrometer (ReTOF-MS) [3]. We will present by the heating of heavily radioactive nuclei, known recent advances that were achieved in laboratory as- as the rapid neutron capture mechanism (r-process trophysics using COSmIC. These include advances heating). The observed thermal glow, known as a in the domain of the diffuse interstellar bands (DIBs) kilonova, can be attributed to the radioactive decay [4, 5] and in the formation of dust grains and aerosols of heavy elements (Rb to U). Unfortunately, there from their gas-phase molecular precursors in envi- is a limited amount of available spectroscopic data ronments as varied as circumstellar outflows [6] and for these elements. The purpose of this research is planetary atmospheres [7, 8, 9]. An extension of to alleviate this problem by using the GRASP01 and the spectral response of the facility into the infrared GRASP2K2, multi-configuration program packages (IR) range is in progress with the addition of a high- which solve the Dirac-relativistic equation, to calcu- resolution near-IR to mid-IR CRDS system that will late atomic energy levels and transition probabilities allow to further investigate cosmic molecules and of the Platinum (Pt) isoelectronic sequence (Pt I, Au grains with COSmIC. Acquisition of laser induced II, Hg III, Tl IV). These findings are compared against fluorescence spectra of cosmic molecule analogs and available theoretical and experimental data3. The Au the laser induced incandescence spectra of cosmic II results are used to simulate emission spectrum to grain analogs are also planned. Preliminary results interpret the Compact Toroidal Hybrid experiment in these fronts will presented and the implications with a gold-plated probe. This work was partially of the on-going studies for astronomy will be ad- supported by NSF grant 1816984. dressed. [1] Dyall et al. Grasp: A general-purpose rela- References: [1] Salama F., et al., Proceedings IAU tivistic atomic structure program. Computer Physics S332, CUP (2018) [2] Biennier et al., Chem. Phys. 326, Communications, 55(3):425–456, 1989. [2] Per Jons- 445 (2006) [3] Ricketts C., et al., Int. J. Mass. Spec. 300, son et al. New version: Grasp2k relativistic atomic 26 (2011) [4] Salama F. et al., The Astrophys. J. 728, structure package. Computer Physics Communi- 154 (2011) [5] Cox, N. et al., A&A 606, A76 (2017) [6] cations, 184(9):2197–2203, 2013. [3] Kramida et al. Contreras, C.S. & Salama, F., ApJ. Suppl. Ser. 208, 6 NIST Atomic Spectra Database (ver. 5.6.1), [Online]. (2013) [7] Sciamma-O’Brien E. et al., Icarus 243, 325 Available: https://physics.nist.gov/asd [2019, (2014) [8] Sciamma-O’Brien E. et al., Icarus 289, 214 April 1]. National Institute of Standards and Tech- (2017) [9] Raymond A.W. et al., ApJ. 853, 107 (2018) nology, Gaithersburg, MD., 2018. Acknowledgements: The authors acknowledge the support of NASA SMD/APRA and SSW pro- 205.04 — Laboratory Astrophysics at NASA Ames: grams and the technical support of E. Quigley. Recent Results and Advances

1 1 205.05 — Rovibrational excitational of diatomic Farid Salama ; Ella Sciamma-O’Brien ; Salma molecules due to H collisions: Waiting for Webb Bejaoui1,2; Lisseth Gavilan1,3; David F. Dubois1,2 2 1 NASA Ames Research Center (Mountain View, California, United Phillip C. Stancil1; Benhui H. Yang1; Yier Wan1; Ziwei States) Zhang1; Robert C. Forrey2; Balakrishnan Naduvalath3; 2 Bay Area Environmental Research Institute, Moffett Field, CA, Peng Zhang4; C. Qu5; J. Bowman5 United States. (Moffett Field„ California, United States) 1 Univ. of Georgia (Athens, Georgia, United States) 3 NPP/USRA (Moffett Field„ California, United States) 2 Penn State Berks Campus (Berks, Pennsylvania, United States) 3 UNLV (Las Vegas, Nevada, United States) The Cosmic Simulation Chamber (COSmIC) facility 4 Duke University (Durham, North Carolina, United States) was developed at NASA Ames to study, in the labo- 5 Emory University (Atlanta, Georgia, United States) ratory, neutral and ionized molecules and nanopar- ticles under the low temperature and high vacuum The expected launch of JWST in 2021 will herald conditions representative of interstellar, circumstel- a new era in astronomy due to its unprecendented lar and planetary environments [1]. COSmIC is com- wavelength resolution and sensitivity in the near in- posed of a Pulsed Discharge Nozzle expansion that frared (NIR). In particular, the NIR Spectrograph generates a plasma in a free supersonic jet expan- (NIRSpec, 0.6-5.3 microns) and the Mid Infrared In- sion coupled to high-sensitivity, complementary in strument (MIRI, 4.9-28.8 microns) will be able to ac-

65 cess a wide range of molecular vibrational bands 205.09 — Radiation temperature characterization which have been heretofore difficult to observe from of a long duration x-ray source for a laboratory the ground. In preparation for modeling JWST ob- photoionized plasma experiment at OMEGA EP

servations of low-density and/or highly irradiated 1 1 1 environments which are out of equilibrium, we have Ryan Schoenfeld ; Roberto Mancini ; Daniel C. Mayes ; Robert F. Heeter2; Duane A. Liedahl2; Sean P. Regan3 performed a series of full-dimensional scattering cal- 1 culations to predict collisional rate coefficients for Physics, University of Nevada, Reno (Reno, Nevada, United States) rovibrational excitation of H2, CO, CN, SiO, CS, and 2 Lawrence Livermore National Lab (Livermore, California, United SO due to the dominant collider H2. In many cases, States) excitations as high as v=5 and/or J=40 have been ob- 3 tained for temperatures as high as 3000 K. The im- Laboratory for Laser Energetics (Rochester, New York, United pact of the new rate coefficients are illustrated with States) NLTE models of typical photodissociation regions, Long duration, i.e. tens of ns, broadband x-ray AGB outflows, and surface layers of protoplanetary sources are important for laboratory photoionized disks. plasma experiments relevant to astrophysics. In a This work was partially supported by NASA series of experiments performed at the OMEGA EP Grants NNX12AF42G, HST-AR-13899.001-A, laser facility, we have used the Gatling-Gun source NNX15AI61G, and NNX16AF09G. to produce an x-ray drive that lasts for 30ns with a radiation temperature Tr =90eV. The Gatling-Gun 205.08 — Radiation cooling in laboratory source is comprised of three Cu hohlraums; each is photoionized plasmas filled with TPX foam and driven by a 10ns- square 1 Roberto Mancini1; Daniel C. Mayes1; Schoenfeld Ryan1; pulsed laser beam with 4.4kJ of UV laser energy . Guillaume Loisel2; James E. Bailey2; Gregory Rochau2; The total source duration of 30ns is achieved by driv- Duane A. Liedahl3 ing the three hohlraums sequentially in time, i.e. 1 University of Nevada, Reno (Reno, Nevada, United States) back-to-back. The radiation temperature was moni- 2 Sandia National Laboratories (Albuquerque, New Mexico, United tored with a VISAR diagnostic to check performance 1 States) and compare with previous miniDMAX data . We 3 Lawrence Livermore National Laboratory (Livermore, California, present measurements of the radiation temperature United States) obtained from VISAR data from two series of experi- ments performed at OMEGA EP, in conjunction with In separate experiments performed at the Z facility of radiation-hydrodynamics simulations of the VISAR Sandia National Laboratories two different samples package. were employed to produce and characterize pho- 1D. Martinez, 2017 Annual OLUG Workshop. toionized plasmas. One was a gas cell filled with This work was sponsored in part by DOE NNSA neon, and the other was a thin silicon/oxygen slab NLUF Grant DE-NA0003533. tamped with plastic. Both samples were driven by the broadband x-ray flux produced at the collapse of a wire array z-pinch implosion. Transmission spec- 206 — iPoster Session: Solar troscopy of a narrowband portion of the x-ray flux Physics Division (SPD), Session II was used to diagnose the charge state distribution, and the electron temperature was extracted from a 206.01 — Investigating Reconnection Evolution Li-like ion level population ratio. We discuss mod- using Si IV Doppler Velocity Measurments eling and results of non-equilibrium atomic physics, 1 1 the effect of the x-ray flux on the atomic level popula- Alysa Derks ; Dana Longcope 1 tion kinetics, and their impact on the radiation cool- Physics, Montana State University (Bozeman, Montana, United ing of laboratory photoionized plasmas. This work States) was sponsored in part by DOE NNSA Grant DE- NA0003875, DOE OFES Grant DE-SC0014451, the Spectroscopic measurements of flare ribbons can Z Facility Fundamental Science Program, and the provide information about the magnetic reconnec- Wootton Center for Astrophysical Plasma Properties. tion process driving the flare. Part of the response of chromospheric material to the energy input from magnetic reconnection, is a redshift known as chro- mospheric condensation. The evolution of this red- shift is related to how long the energy was deposited

66 for, and the spatial scale of where the energy was portions of the duration of each flare, and we inter- deposited in the corona. In this study, we use In- pret our results in the context of the standard solar terface Region Imaging Spectrograph (IRIS) FUV ob- flare model involving magnetic energy release, mag- servations of a flare on October 25, 2014 to measure netic reconnection, and particle acceleration. Doppler shifts of the Si IV 1402 and 1393 Å lines and the time evolution of each line. Both Si IV lines are 206.03 — High Resolution Post-flare Loop well fit using a sum of two Gaussian components. Observations by GST and IRIS Here, we have developed a fitting procedure which 1 1 1 1 will directly infer the Doppler velocity of the red and Nengyi Huang ; Yan Xu ; Ju Jing ; Haimin Wang 1 blue shifted component at each non-saturated ribbon New Jersey Institute of Tech (Newark, New Jersey, United States) pixel. We see that these red and blue shifted com- ponents peak to a maximum velocity and then de- We present the study of post-flare loops, during the cay away to its normal velocity. This is the behav- gradual phase of the 2015-06-22 M6.5 two-ribbon ior predicted by models of chromospheric conden- flare, which was observed by Goode Solar Tele- sation (Fisher et al. 1985, Longcope 2014). Using re- scope (GST) and Interface Region Imaging Spectro- sults from this study, we seek evidence for the re- graph (IRIS). Imaging spectroscopic data in UV and connection length scale and the reconnection spatial Hα lines are analyzed, with supplementary data of dependence. This work is supported by a grant from magnetograms and EUV images. We compare the NSF/AST. Doppler signals derived from Mg II 2791.59 Å, Si IV 1402.77 Å with those derived from Hα line to study 206.02 — Statistical analysis of evolving flare the mass motions in the transition region and chro- parameters inferred from spatially-resolved mosphere. In addition, Hα images are used for trac- microwave spectra observed with the Expanded ing the structure and mass motion in loops. Further- Owens Valley Solar Array more, we investigate the oscillations of flare loops in Fe XXI 1354.08 Å and Hα lines. Finally, we compare 1 1 1 Gelu M. Nita ; Gregory D. Fleishman ; Dale E. Gary ; our diagnostics with the results of flare loop model- 1 1 2 Bin Chen ; Sijie Yu ; Natsuha Kuroda ing. 1 New Jersey Institute of Technology (Newark, New Jersey, United States) 2 University Corporation for Atmospheric Research (Boulder, Col- 207 — iPoster Session: Stars & orado, United States) Friends I The newly completed Expanded Owens Valley Solar Array (EOVSA) performed microwave (MW) imag- 207.01 — Intel Secure Key-Powered Radio-flaring ing spectroscopy observations during several flares Ultracool Dwarf Population Synthesis that occurred during the first half of September 2017. Matthew Route1 The unprecedented high frequency and spatial res- 1 Purdue University (West Lafayette, Indiana, United States) olution of these observations allowed us for the first time to infer, with 2-arcsecond spatial resolution and Over a dozen ultracool dwarfs (UCDs), which in- 1-second temporal cadence, the spatial distribution habit the boundary between low mass stars and and evolution of the coronal magnetic field strength, brown dwarfs, are known sources of radio activity. the number density of the accelerated electrons, the This activity consists of highly (∼100%) circularly power-law index of their energy distribution, as well polarized, high brightness temperature radio flares as other associated flare parameters. Our method- thought to be caused by the electron cyclotron maser ology, which consists of independently fitting the operating in kG magnetic fields. Using the statistical MW spectra corresponding to each individual pixel properties of the population of UCDs know thus far of the evolving mult-frequency maps with uniform together with well-characterized instrumentation at gyrosynchrotron source models, generated a statisti- , a Monte Carlo simulator may cally significant collection of evolving flare parame- be constructed to gain insight into this intriguing ters whose generally smooth spatial and time varia- class of objects. This simulator is powered by Intel tion demonstrates a collective behavior of the neigh- Secure Key, also known as the RdRand instruction boring volume elements, and thus validates our ap- set, which is a new processor technology that uses proach. Here we report on the statistical properties a local entropy source to improve random number of these physical flare parameters, their spatial dis- generation that has heretofore been used to improve tributions, and their temporal trends for significant

67 cryptography. The simulations indicate that only measured by the All Sky Automated Survey (ASAS). ∼5% of radio-flaring UCDs within the local neigh- Based on these initial observations, eight targets have borhood have been discovered thus far, with another been chosen for dedicated spectroscopic and photo- ∼40 remaining to be discovered within 25 pc of the metric study. We present the current status of eight Sun. We review potential reasons for this success targets with regard to photometric observations ob- rate, and also assess the performance of the ISK tech- tained at The BB&T Observatory of Thomas More nology. University. We also provide initial estimates of the system parameters for those binaries with sufficient 207.02 — Lightcurve Asymmetries in KEPLER & spectroscopic and photometric observations for bi- TESS Eclipsing Binaries nary modeling. Brent Koogler1; Jordan Shroyer1; Vayujeet Gokhale1 1 207.04 — Recombination Energy and Common Truman State University (La Salle, Illinois, United States) Envelope Ejections In this work, we study the O’Connell effect which Jingyao Zhu1; Paul M. Ricker1; Frank Timmes2; Ronald describes the asymmetry in the out of eclipse max- Taam3,4; Ronald F. Webbink1 ima in Eclipsing Binary (EB) systems found in the 1 Astronomy & Physics, University of Illinois at Urbana Cham- Kepler and TESS fields. We calculate a Lomb-Scargle paign (Urbana, Illinois, United States) Periodogram for each object, and fit the resulting 2 Arizona State University (Tempe, Arizona, United States) phase folded data with a twelve term Fourier fit. For 3 Northwestern University (Evanston, Illinois, United States) each orbital cycle, the Fourier coefficients are used 4 Academia Sinica (Taipei, Taiwan) to quantify the asymmetry in the light curves by cal- culating the ‘Lightcurve Asymmetry’ (LCA) and the Hydrodynamical simulations of binary systems un- ‘O’Connell Effect Ratio’ (OER). We describe the time dergoing common envelope evolution have gener- evolution of these asymmetries in hundreds of EBs. ally failed to achieve the levels of envelope ejec- We generate starspot models for these systems us- tion and orbital inspiral needed to produce observed ing the eclipsing binary modeling software Binary post-common envelope binaries, particularly binary Maker 3 (Bradstreet, 2005) and PHOEBE (Prsa, 2016), white dwarfs. Energy released by hydrogen and/or to test the hypothesis that the asymmetries are due to recombination in the expanding envelope the presence of starspots on one or both components has been invoked as a potential source of energy, of the binary. Additionally, we classify each sys- and recently Nandez and Ivanova have found us- tem as either Algol-type (EA), Beta-Lyrae type (EB), ing smoothed particle hydrodynamics (SPH) sim- W-UMA type (EW), or as an ‘irregular’-type system ulations that this mechanism may work if the en- based on the criteria set by Rucinski (1997). Finally, ergy can be trapped and used to do work. How- we report on any correlation between the lightcurve ever, it is not clear whether this condition actually asymmetries and eclipsing binary type. obtains in real systems. In particular, the efficiency of energy transport in removing this energy needs 207.03 — Continuing Investigation of Eclipsing to be evaluated, as well as potential dynamical in- Binaries at The BB&T Observatory of Thomas stabilities triggered by the existence of partial ion- More University ization zones, which could change the ejection cri- terion. To gain insight into this question, we are 1 1 1 Raymond Whitehill ; Kylie Anderson ; Wesley Ryle ; conducting adaptive mesh refinement (AMR) sim- 1 1 1 Kelsey Etherton ; Cristi Farwick ; Sierra O’Bryan ; ulations of common envelopes with radiation diffu- 1 Terri Perrino sion and an that includes hydrogen 1 Mathematics and Physics, Thomas More University (Crestview and helium partial ionization. We present simula- Hills, Kentucky, United States) tions of red giant- systems, with param- eters similar to those studied by Nandez et al., which Eclipsing binaries are an ideal source of direct and are proposed as potential progenitors of the double- precise measurements of stellar parameters. This white dwarf system WD 1101+364. We discuss the ongoing study focuses on a subset of eclipsing bi- efficiency of envelope ejection in these systems, ex- nary systems of intermediate mass (roughly 3M⊙ to amining its connection to the relative locations of the 10M⊙). High precision measurements of stellar pa- photosphere and partial ionization zones. rameters for this subset are rare, despite the impor- tance of these stars in a variety of astrophysical phe- nomenon. Targets were identified based on varibility

68 207.05 — A Search for X-ray Emitting Binary Stars Nora Hänni1; Martin Rubin1; Thierry Semon1; Susanne in the Core of Omega Centauri Wampfler1 1 University of Bern (Bern, Switzerland) 1 1 1 Kyle Murphy ; Adrienne Cool ; Sarah Deveny ; Andrea 2 Universite Pierre et Marie Curie (Paris, France) 2 2 Bellini ; Jay Anderson 3 Institut Royal Belge d’Aéronomie Spatiale (Brussels, Belgium) 1 San Francisco State University (San Francisco, California, United 4 Southwest Research Institute (San Antonio, Texas, United States) States) 5 University of Texas at San Antonio (San Antonio, Texas, United 2 Space Telescope Science Institute (Baltimore, Maryland, United States) States) 6 University of Michigan (Ann Arbor, Michigan, United States)

We have searched for optical counterparts of Chan- Containing some of the most pristine material in our dra sources within the core of the solar system, comets are unique objects of study: Omega Centauri utilizing a catalog of photometry Their slow formation in the outer region of the pro- and proper motions derived from over 650 Hubble toplanetary disk protected them from high temper- Space Telescope WFC3/UVIS exposures (Bellini et atures and led to preservation of the original ma- al. 2017). A total of 67 X-ray sources lie within terial that had formed our solar system. Thus, the field of view of these HST images, 25 ofwhich profound understanding of the chemical composi- were reported for the first time by Henleywillis et tion of comets has the potential to provide answers al. (2018). Using a subset of six wide-band filters for fundamental scientific questions such as evolu- (F225W, F275W, F336W, F438W, F606W, and F814W) tion of our solar system or how life emerged on and two H-α filters (F656N and F658N), we construct Earth. However, decryption of the chemical com- color-magnitude diagrams to search for stars in the position of comets is difficult. Spacecraft observa- X-ray error circles whose properties are indicative tions often consist of single encounters at relatively of binarity, e.g., cataclysmic variables, coronally ac- large distances only and even ground-based obser- tive binaries (BY Dra or RS CVn systems), and sub- vational methods appear to be limited for some or- or red stragglers. We identify ten new bi- ganic molecules due to weak dipole moments. A nary candidates and recover seven previously iden- new scientific approach was established when the tified systems, providing independent confirmation spacecraft was sent to comet Churyumov- that the latter have the properties expected of bina- Gerasmienko (67P). For the first time a spacecraft ries. The binary candidates comprise nine candidate performed in-situ measurements of the and cataclysmic variables, five possible BY Dra systems, nucleus while accompanied the comet on its way and three red stragglers, two of which may be associ- around the Sun. Onboard the spacecraft, the Rosetta ated with the metal-rich anomalous giant or Orbiter Spectrometer for Ion and Neutral Analysis branches of Omega Centauri. We also find evidence (ROSINA) determined the chemical composition of that four of the X-ray sources are foreground stars the volatiles in the coma at various distances and an- and two are probable active galactic nuclei in the gles between comet, Sun, and spacecraft, from ar- background. We discuss the significance of these re- rival at the comet in 2014 until the final landing in sults in the context of efforts to understand the over- 2016. Based on these data, the existence of a sur- all binary content and X-ray emissivity of globular prising amount and complexity of organics in the clusters. (semi-)volatile phase of the comet was demonstrated, with some molecules being detected for the first time 208 — iPoster Session: ever in comets. After revealing this unexpected com- plexity, a key step in decryption of the exact com- Instrumentation Space, Ground position was made by deriving the CH- and CHO- and Computation composition from the DFMS space data. The study presented here uses data from the ROSINA Dou- ble Focusing Mass Spectrometer and combines lab- 208.01 — CH- and CHO-Composition in Comet oratory calibration at the Bernese calibration facility 67P/Churyumov-Gerasimenko revealed by the (CASYMIR) and space data analysis. This combi- Rosetta Mission nation produces the first detailed identification and Markus Schuhmann1; Kathrin Altwegg1; Hans quantification campaign of CH- and CHO-bearing Balsiger1; Jean-Jacques Berthelier2; Johan De Keyser3; molecules in comet 67P. The results are compared Stephen Fuselier4,5; Sebastien Gasc1; T. I. Gombosi6; to measurement and modelling results from other comets and the interstellar medium.

69 208.02 — WFIRST: Project Overview and Status 208.04 — Recent Scientific Highlights from the

1 Stratospheric Observatory for Infrared Astronomy Jeffrey W. Kruk (SOFIA) 1 NASA - GSFC (Greenbelt, Maryland, United States) Arielle Moullet1; Randolf Klein1 The Wide-Field InfraRed Survey Telescope (WFIRST) 1 SOFIA/USRA (Moffett Field, California, United States) will be the next Astrophysics strategic mission to follow JWST. The observatory payload consists of The Stratospheric Observatory for Infrared Astron- a Hubble-size telescope aperture with a wide-field omy (SOFIA) is currently the only observing fa- NIR instrument and a coronagraph operating at vis- cility offering a window into the whole mid- and ible wavelengths that employs state-of-the-art wave- far-IR spectrum (5-600 microns). Its ever evolving front sensing and control. The Wide-field instrument suite of instruments offers high-speed mapping, low is optimized for large area NIR imaging and spec- and high-spectral resolution modes (up to R=108), troscopic surveys, with performance requirements and recently added polarimetric capabilities on the driven by programs to study cosmology and exo- HAWC+ far-IR camera. This unique and upgrad- planet detection via gravitational microlensing. All able set of instruments, combined with the abil- data will be public immediately, and substantial gen- ity for the telescope to target Northern and South- eral observer and archival research programs will be ern sources, makes SOFIA an essential facility for supported. The WFIRST Project is presently in Phase the astrophysics community, highly complementary B, with the confirmation review expected in late 2019 to HST/JWST and ALMA. Over 6 observing cy- or early 2020. Candidate observing programs are un- cles, SOFIA observations have targeted very diverse der detailed study in order to inform the mission de- sources such as Solar System objects, young stellar sign, but the actual science investigations will not be objects and disks, planetary nebulae, star-forming selected until much closer to launch. We will present regions (galactic and extra galactic) and AGNs. Such an overview of the present mission design and ex- observations address a variety of science cases, in- pected performance, a summary of Project status, cluding the morphology of magnetic fields on galac- and plans for selecting the observing programs. tic scales, ISM gas chemistry, PAH spectroscopy, and atomic/ionized emission in massive star-forming re- 208.03 — High Energy Exoplanet Science in the gions. This poster summarizes the most recent high- Next Decade and Beyond profile SOFIA-enabled scientific results, focusing on dust imaging and polarimetry in nearby active galax- 1 Scott J. Wolk ies, supernovae remnants, and galactic star-forming 1 SAO (Cambridge, Massachusetts, United States) regions. The two large proposals recently accepted through the Legacy Science Proposal, which aims I present a comparison of high energy studies of ex- at providing high-value products to the astronomi- oplanet targets which can be done with the next gen- cal community, will also be described. Finally, we eration of X-ray telescopes. Specifically, I will show present the capabilities of HIRMES, the third genera- the immediate and decisive impact of XRISM, SEEJ tion mid/far-IR imager and spectrometer instrument and Athena. Future studies will focus increasingly planned for commissioning in 2020, and HIRMES’ on other planetary systems and the exoplanet science future contribution to the study of the mass and com- which comes from understanding the interactions position (including ice and gas-phase water content) between the stellar magnetic fields and the planetary of protoplanetary disks. magnetic fields. Observations enabled by planned grating spectrometers such as those aboard Arcus 208.05 — Absolute flux calibration and and Lynx will allow us to capture dynamic changes characterization of the SOFIA FIFI-LS integral in these environments, furthering our knowledge of field spectrometer. the energetic side of stellar ecosystems. By the late 2020’s and 2030’s characterization of the high energy Dario Fadda1; William D. Vacca1; Christian Fischer2; environments of specific exoplanets will be a neces- Sebastian Colditz2; Robert F. Minchin1; Randolf Klein1 sary step in our evaluation of their current and fu- 1 USRA (Moffett Field, California, United States) ture prospect for habitability. All four of these mis- 2 DSI (Stuttgart, Germany) sions will be able to uniquely contribute to our un- derstanding of these systems. We present the absolute flux calibration and char- acterization of the Far-Infrared Field-Integral Line Spectrometer (FIFI-LS ) of SOFIA. The work is based

70 on observations made in the laboratory with an inter- observed from space due to significant telluric ab- nal calibrator and on observations of planets, moons, sorption from the Earth’s surface. In order to mea- and as absolute flux calibrators made in the sure the CO2 production rate, we carried out a coor- last 5 years. Two sets of responses are presented, be- dinated observing campaign using the Arizona Ra- fore and after the filter window change made at the dio Observatory Submillimeter 10-m telescope, the end of 2017 to improve the sensitivity at 52 μm. IRAC instrument on the Spitzer Space Telescope, The relative spectral response of each detector of iSHELL on the NASA IRTF, and the Institut de Ra- the FIFI-LS arrays is derived using the internal cal- dioastronomie de Millimetrique 30-m telescope dur- ibrator while the illumination of the arrays is esti- ing January-February 2018. CO was strongly de- mated through sky flats. The linearity of the array tected from the ground-based spectra and there is response was studied using several observations of a very strong presence of gaseous emission in the bright sources. 4.5 micron IRAC channel, which is sensitive to both We find that the deviation from linearity of the CO2 and CO emission. We completed a compre- FIFI-LS arrays is typically less than 1%. The flux hensive analysis of the SMT, iSHELL, and IRAM ob- calibration accuracy is estimated to be 10% or better servations in order to estimate the CO contribution across the entire wavelength range of the instrument. to the observed Spitzer 4.5 micron channel fluxes. Repeatability of better than 5% is found though mul- This is crucial to extract the CO2 abundance from tiple measurements of the same calibration source. the Spitzer imaging. We will present and discuss our CO and CO2production rates, and explain our 208.06 — A Coordinated Ground- and Space- program to measure pre-perihelion (Feb 2018) and Based Observing Campaign to Measure CO2and post-perihelion (June 2019) values of the CO2/CO ra- CO Emission in C/2016 R2 (PANSTARRS) tios. This work makes use of Director’s Discretionary Time observations obtained on Spitzer, IRTF, ARO, 1 3 3 Olga Harrington ; Adam McKay ; Michael A. DiSanti ; and IRAM and we thank these observatories for 4 2 Michael S. Kelley ; Anita L. Cochran ; Neil Dello granting our group DDT time to conduct these obser- 5 6 1 Russo ; Maria Womack ; Kacper Wierzchos ; Nico- vations. This work is funded through the NASA NPP 7 4 5 las Biver ; James M. Bauer ; Ronald J. Vervack ; Bon- program, administered by USRA, by NSF grant AST- 8 9 9 cho P. Bonev ; Erika L. Gibb ; Nathan Roth ; Hideyo 1615917 to M.W. and a Genshaft Family Doctoral Fel- 10 Kawakita lowship to O.H.P. 1 University of South Florida (Tampa, Florida, United States) 2 Kyoto Sangyo University (Kyoto, Japan) 3 208.07 — Multibeam Receiver System and Key McDonald Observatory (Ft. Davis, Texas, United States) Science Programs of TRAO 4 NASA GSFC/USRA (Greenbelt, Maryland, United States) 5 University of Maryland (College Park, Maryland, United States) Youngung Lee1 6 JHU-APL (Laurel, Maryland, United States) 1 Radio Division, Korea Astronomy and Space Science Institute 7 University of Central Florida (Orlando, Florida, United States) (Deajeon, Korea (the Republic of)) 8 Obs. de Paris (Montparnasse, France) 9 American University (Washington, District of Columbia, United Taeduk Radio Astronomy Observatory (TRAO) is States) equipped with a main control computer with Vx- 10 University of Missouri-St. Louis (St. Louis, Missouri, United Works operating system, a new receiver system, States) and a new backend system. The new receiver system(SEQUOIA-TRAO) is equipped with high- Comets are similar to time capsules in that they give performing 16-pixel MMIC pre-amplifiers in a 4x4 hints about the characteristics of the solar system as array, operating within 85∼115 GHz frequency it was forming. They are composed of rock, dust, range. The system temperature ranges from 150 K water ice, frozen carbon dioxide, carbon monoxide, (85 GHz) to 400 K (115 GHz). The 2nd IF modules methane, and ammonia, where there is typically with the narrow band and the 8 channels with 4 FFT more carbon dioxide (CO2), than carbon monoxide spectrometers allow to observe 2 frequencies simul- (CO). Comet C/2016 R2 is a special example of a taneously within the 85∼100 or 100∼115 GHz bands comet that produced an unusual chemical compo- for all 16 pixels of the receiver. Radome replacement sition profile, with large amounts of CO, CO+,N2+ was completed successfully as of February 2017. In with very little else (McKay et al. 2018; Wierzchos addition, a new servo system will be installed in & Womack 2018; Biver et al. 2018). CO2 is also 2017 summer. We provide OTF (On-The-Fly) as a often abundant in comets; however, it can only be main observing mode, and position switching mode

71 is available as well. The backend system (FFT spec- Moreover it can be transported the planets images trometer) provides the 4096x2 channels with fine ve- to a broadband spectrometric instrument that able to locity resolution of about 0.05 km/sec (15 kHz) per investigate the constituent of the . channel, and their full spectra bandwidth is 60 MHz. Beam efficiency of the TRAO was measured tobe 208.09 — The Preliminary CatWISE Catalog about 46% – 54% (with less than 2% error) between 1 85 and 115 GHz bands and pointing errors of the Peter R. Eisenhardt 1 14m telescope were found be 4.4 arcsec in AZ direc- JPL/Caltech (Pasadena, California, United States) tion and 6 arcsec in EL direction. Generally, we al- locate 18 hours of telescope time a day from January The Preliminary CatWISE catalog consists of to the middle of May, and from October to Decem- 957,285,574 sources over the entire sky selected from ber. Three Key Science Programs had been selected WISE and NEOWISE survey data at 3.4 and 4.6 in 2015 fall and they are supposed to have higher pri- microns (W1 and W2) collected from 2010 to 2016. ority for telescope time. We welcome and support This dataset includes four times as many exposures invaluable observation programs. and spans over ten times as large a time baseline as the AllWISE catalog. CatWISE adapts AllWISE software to measure the sources in co-added images 208.08 — Evaginated Apodization Coronagraph created from six month subsets of these data, each Jaeho Choi1; Junho Cha1 representing one coverage of the inertial sky, or 1 Physics, Dankook University (Cheonan, Dongnam-ku, Korea (the epoch. The catalog includes the measured motion Republic of)) of sources in 8 epochs over the 6 year span of the data. From comparison to Spitzer, the SNR 5 Vega High contrast imaging of faint objects nearby the magnitude limits are W1=17.58 and W2=16.43, bright objects is a challenging task due to it requires vs. W1=16.90 and W2=15.95 for AllWISE. From a high angular resolution and high dynamic range comparison to Gaia, the motions are ten times more detections concurrently. For imaging older and less accurate than those from AllWISE. The Preliminary massive are required spectroscopic and achromatic CatWISE catalog is available to the astrophysics high contrast imaging. Moreover, large broadband community at https://catwise.github.io. is extreme challenging in visible and near-infrared. The coronagraph coupled with extreme adoptive op- 208.10 — Searching for Low-mass Stellar and tics is being operated to a high-contrast imaging for a Sub-stellar objects in the JWST North Ecliptic direct observation of exoplanets which will provide Pole Time-Domain Field their chemical composition of atmospheres and their temperature. The essential scheme of the EAC is that Thomas Tyburczy1; Rolf A. Jansen1; Rogier A. the apodization carried out by excluding evaginated Windhorst1; Teresa Ashcraft1,2; William D. Cotton3; images after passing a set of axicon lenes. The pre- Christopher Willmer4; Norman A. Grogin5; Cameron requisite of completely evaginated of the entire en- White1 trance pupil of the EAC is that the distance between 1 Arizona State University (Tempe, Arizona, United States) two ALs should be setting the refracted beam at the 2 Michigan State University (East Lansing, Michigan, United close to the apex of the first AL is reached to the out- States) most surface rim of the given second AL. Once this 3 National Radio Astronomy Observatory (Charlottesville, Virginia, condition is satisfied, the central bright star light has United States) been so relocated to the rim of the image which is 4 University of Arizona (Tucson, Arizona, United States) easy to cut off by a variable aperture iris, thoroughly 5 Space Telescope Science Institute (Baltimore, Maryland, United without losing any image of the faint objects. The States) laboratory based axicon-lens coronagraph imaging support the symbolic computation results which has The James Webb Space Telescope (JWST) North Ecliptic potential in direct imaging for finding exoplanet and Pole (NEP) Time-Domain Field (TDF) is a 14’ diam- various astrophysical activities. We report, an evagi- eter region of the sky selected to be ideal for ultra- nated apodization coronagraph(EAC) method using deep (mAB ∼ 29 mag) time-domain science with the axicon-lenses, which achieve the small IWA and JWST (Jansen & Windhorst 2018), that is being devel- high contrast imaging with large broadband imaging oped as a community field. Located within JWST’s in visible to near-infrared. Furthermore it insensitive northern Continuous Viewing Zone, it can be ob- to the stellar angular size and the setup of the coro- served year-round, is devoid of detector saturating nagraph is simple to build and is durable to operate. stars, has low Galactic foreground extinction, and

72 will be targeted by GTO program 1176 (Windhorst) induces an oppositely directed electric current in the with NIRCam and NIRISS. It is the only region in background plasma; this eddy current is required to the sky where JWST can observe a clean extragalactic satisfy the frozen-in magnetic flux condition in the deep survey field of this size at arbitrary cadence and background plasma. The magnetic force between orientation, enabling a wide range of new and ex- the inner-core electric current and the oppositely di- citing time-domain science, including high redshift rected induced eddy current propels the background transient searches and monitoring (e.g., SNe), vari- plasma away from the core, creating a cavity and a ability studies from Active Galactic Nuclei (AGN) to density pileup at the cavity edge. The cavity radius brown dwarf atmospheres, as well as proper motions saturates when an inward restoring force from mag- of extreme scattered Objects and comets netic and hydrodynamic pressure in the region out- beyond the distance of , and of nearby side the cavity edge balances the outward magnetic Galactic brown dwarfs, low-mass stars, and ultracool force. The model is supported by (i) laboratory ex- white dwarfs. In anticipation of JWST’s launch in periments showing the development of a cavity as a 2021, a wealth of ancillary data across the electro- result of the repulsion of an induced reverse current magnetic spectrum (X-ray–radio) has already been by a rising inner-core flux-rope current, (ii) 3D nu- collected. This includes deep (∼0.9 muJy rms) VLA merical magnetohydrodynamic (MHD) simulations 3GHz radio observations (B+A configuration) and that reproduce the laboratory experiments in quanti- LBT/LBC Ugrz (mAB ∼ 26 mag) and MMT/MMIRS tative detail, and (iii) an analytic model that describes YJHKs (mAB ∼ 24.5–22 mag) photometry of the en- cavity formation as a result of the plasma containing tire JWST NEP TDF, as well as HST/WFC3+ACS the induced reverse current being repelled from the UV–Visible observations of the central r<∼5’. Since inner core. This analytic model has broad applicabil- a major science driver for this field is the study of ity because the predicted cavity widths are relatively AGN activity, and since Galactic late-type stars and independent of both the current injection mechanism brown dwarfs are often identified within samples of and the injection timescale. AGN candidates, we here report on an analysis of the 3GHz radio and LBT/LBC and MMT/MMIRS 209.03 — Laboratory plasma experiments to test visible–near-IR observations to search for such late- photoionized plasma models type stellar and substellar sources. We also aim to 1 1 2 study their properties, with particular emphasis on Daniel C. Mayes ; Roberto Mancini ; James E. Bailey ; 2 2 the possible detection of faint radio-emission (coro- Guillaume Loisel ; Gregory Rochau 1 nal, auroral, flares) of either individual objects or Physics, University of Nevada - Reno (Reno, Nevada, United (through stacking) of the populations. We further- States) 2 more report on the progress of HST-GO-15278, the Sandia National Laboratories (Albuquerque, New Mexico, United final two visits of which executed flawlessly, andpre- States) liminary analysis thereof. We discuss an experimental effort to create and study astrophysically relevant photoionized plasmas in the 209 — iPoster Session: Laboratory laboratory. Conditions relevant to the extreme en- vironments in x-ray binaries, accretion disks around Astrophysics Division (LAD) black holes, and active galactic nuclei have long been experimentally inaccessible. Astronomers looking to 209.01 — Reverse Current Model for Coronal Mass understand such objects rely on the accuracy of the Ejection Cavity Formation photoionization models they employ, yet we are only Magnus Albert Haw2,1; Pakorn Wongwaitayakornkul2; beginning to have the ability to probe this regime ex- Hui Li3; Paul M. Bellan2 perimentally with devices such as the Z-Machine at 1 TNP, NASA Ames Research Center (Moffett Field, California, Sandia National Laboratories. Our experiment uti- United States) lizes the intense x-ray flux emitted at the collapse 2 Caltech (Pasadena, California, United States) of a Z-pinch to heat and backlight a neon photoion- 3 Los Alamos Nat’l Laboratory (Los Alamos, New Mexico, United ized plasma contained within a cm-scale gas cell 17 18 −3 States) with atom number densities of 10 to 10 cm . The broadband x-ray flux at the gas cell at the peak We report here a new model for explaining the three- of the x-ray drive is of order 1012 W/cm2 produc- part structure of coronal mass ejections (CMEs). The ing an order of magnitude range in ionization pa- model proposes that the cavity in a CME forms be- rameter from about 5 to 50 erg*cm/s, depending cause a rising electric current in the core prominence

73 on gas fill pressure. The resulting plasma condi- computed and compared against available theoreti- tions are determined using K-shell line absorption cal and experimental data [3]. The Au IV results are spectroscopy from a KAP crystal spectrometer ca- used to simulate emission spectrum to interpret the pable of capturing both time-integrated and time- Compact Toroidal Hybrid experiment with a gold- gated transmission spectra. Analysis of these spec- platted probe. This work was partially supported by tra yields ion areal densities and the charge state dis- NSF grant 1816984 tribution, which can be compared with simulation [1] Dyall, et al., Computer physics communica- results from atomic kinetics codes. In addition, the tions, 55(3):425–456, 1989 [2] Per Jonsson, et al., electron temperature is extracted from level popu- Computer Physics Communications, 184(9):2197– lation ratios of nearby energy levels in Li-like ions, 2203, 2013 [3] Kramida, et al. NIST Atomic Spec- which can be used to test heating models of pho- tra Database, https://physics.nist.gov/asd [4] toionized plasmas as well. Parpia, et al., Computer physics communications, This work was sponsored in part by DOE NNSA 94(2-3):249–271, 1996 HEDLP grant DE-NA0003875, DOE Office of Science Grant DE-SC0014451, the Wootton Center for Astro- 209.05 — Measuring the 15N(α,γ)19F reaction physical Plasma Properties, and the Z Facility Fundamen- using a Bubble Chamber. tal Science Program of SNL. David Neto1; Kevin Bailey2; Jay F. Benesch3; Brandi 3 2 3 209.04 — Relativistic Atomic Structure of the Au Cade ; Brad DiGiovine ; Joseph M. Grames ; Alicia Hofler3; Roy Holt4; Reza Kazimi3; Dave Meekins3; IV Isoelectronic Sequence: opacity data for 3 3 2 kilonova ejecta Daniel Moser ; Mathew Poelker ; Tom O’Connor ; Karl Rehm2; Seamus P. Riordan2; Riad S. Suleiman3; Rashi Zahra Taghadomi1; Yier Wan1; A. Flowers1; P. Stancil1; Talwar2; Claudio Ugalde1 Brendan McLaughlin2; S. Loch3; S. Bromley4; J. P. 1 Physics, University of Illinois at Chicago (Chicago, Illinois, Marler4; C. E. Sosolik4 United States) 1 Department of Physics and Astronomy, Center for Simulational 2 Argonne National Laboratory (Lemont, Illinois, United States) Physics, The University ofGeorgia (Athens, Georgia, United States) 3 Jefferson Lab (Newport News, Virginia, United States) 2 Centre for Theoretical Atomic and Molecular Physics (CTA- 4 Caltech (Pasadena, California, United States) MOP), School of Mathematics andPhysics, Queen’s Universit (Belfast, United Kingdom) Radiative capture reactions, such as (α,γ), (p,γ) and 3 Department of Physics, Auburn University (Auburn, Georgia, (n,γ), are of fundamental importance to the study United States) of nucleosynthesis of elements in stellar cores, su- 4 Department of Physics, Clemson University, 104 Kinard Labora- pernovae, etc. In the laboratory, these reactions are tory, (Clemson, Georgia, United States) usually measured by bombarding gas targets or very thin films with particle beams. The low density of Direct detection of gravitational waves (GW) on Aug. these targets and the sensitivity to background from 17, 2017, propagating from a binary neutron star environmental and cosmic sources can lead to long merger, opened the era of GW astronomy. The running times. In this contribution we explain a ejected material from neutron star mergers is called method - using a single fluid bubble chamber to mea- “kilonova” or “macronova” which is a good candi- sure nuclear reaction cross sections. Here determin- date for optical and near infrared follow-up observa- ing the cross section of the 15N(α,γ)19F reaction rel- tions after the detection of GWs. The kilonova pro- evant to the synthesis of fluorine in AGB stars (pos- vided the first direct evidence for the synthesis of sibly also in Wolf-Rayet stars). The higher density heavy nuclei through the rapid neutron capture pro- of the fluid and measuring the time-reversed reac- cess or so called r-process. Although properties of tion increases the luminosity of the experiment by the emission are largely affected by opacities in the several orders of magnitude. We have measured ejected material, available atomic data for r-process the cross section of the photodisintegration process elements are still limited. The aim of our research is 19F(γ,α)15N by bombarding a superheated fluid of to alleviate this situation, in this regard we are us- C3F8 with Bremsstrahlung γ rays produced from ing GRASP0 [1,4] and GRASP2K [2] to obtain en- the electron injector at Jefferson Laboratory reaching ergy levels and transition properties then generate cross sections of the time-reversed 15N(α,γ)19F reac- reliable line lists for a range of r-process elements tion of about 80 picobarn. (Re-Pt). Here, Au IV, as well as its low-charged iso- This work was supported by the US Department electronic sequence members, Os I, Ir II, Pt III, , are of Energy, Office of Nuclear Physics, under Contracts

74 No. DE-AC02-06CH11357 (ANL) and No. DE-AC05- instrumentation for future space exploration mis- 06OR23177 (JLAB). sions. The Jovian moon is of particular in- terest for the search of within our 209.06 — Searching for Contemporary Supernova solar system. At NASA’s Jet Propulsion Laboratory, Dust in Deep-Sea Sediments we have used the two-color Laser Ablation Ioniza- tion Mass Spectrometer system to study such ice- 1 1 1 Ryan Christopher Ogliore ; Nan Liu ; Heng Chen ; Kun surface analogues.1,2 The system has the capabilities 1 Wang to simulate relevant conditions, encountered in rele- 1 Physics, Washington University in St. Louis (Saint Louis, Mis- vant environments. The structure of the ice depends souri, United States) on the deposition temperature. IR laser desorption combined with multi-photon ionization mass spec- The short-lived radioisotope 60Fe is synthesized pre- trometry, provides insights in the desorption dy- dominantly in supernovae and is not produced effi- namics of the plume. We are capable of varying the ciently by other mechanisms like cosmic-ray spalla- wavelength of the IR laser, from 2700-3100 nm. By tion. An excess of 60Fe has been detected in deep-sea introducing different species in low abundances into sediments, ferromanganese crusts, and in Apollo 12 the ice structure, we can study if these molecules fol- lunar soils. These measured excesses in 60Fe are con- low the same trend in extraction time as the water sistent with an injection from a nearby supernova ∼2 molecules. These fundamental investigations are es- Myr ago. sential for understanding the processes at play, and The solar wind and interplanetary magnetic field gaining insights into the nanosecond laser-induced would have effectively shielded the Solar System desorption process. from gas and plasma ejected from a nearby super- 1. Henderson, B.L. and Gudipati, M.S., The Jour- nova, so it was likely supernova dust grains that nal of Physical Chemistry A, V.118, I.29. (2014) 2. carried the 60Fe signature to Earth and the Moon. Paardekooper, D.M. et al. Rev. Sci. Instrum., 85, Graphite and silicon-carbide dust grains from this 104501. (2014) supernova, phases that are well-studied in super- nova grains that predated the formation of the Solar System, would have likely survived atmospheric en- 210 — iPoster Plus VI: (SPD), try. These grains would represent an extremely valu- able sample of contemporary supernova dust that Flares can be studied using high-precision laboratory tech- niques and compared to presolar (>4.6 Gyr old) su- 210.01 — On the Origin of Quasi-periodic pernova dust. Fast-mode Propagating Wave Trains (QFPs): A Here we describe our efforts to identify contempo- Statistical Survey rary supernova dust in deep-sea sediments. Jay Silver1; Wei Liu1; Leon Ofman2 1 Lockheed Martin Solar and Astrophysics Laboratory (Palo Alto, 209.07 — Plume profile studies of nanosecond California, United States) laser-induced desorption of water ice - amorphous 2 Catholic University of America (Washington, District of versus crystalline - Columbia, United States) 1 1 Daniel Paardekooper ; Bryana Lynne Henderson ; The magnetized solar corona hosts a variety of waves Murthy Gudipati1 1 that are physically important and can serve as useful Science, Jet Propulsion Laboratory (Pasadena, California, United diagnostic tools. One type of such coronal waves are States) Quasi-periodic Fast-mode Propagating wave trains (QFPs), which were first detected in extreme ultra- In the interstellar medium and within our solar sys- violet (EUV) by the Atmospheric Imaging Assem- tem, ice is present in diverse locations ranging from bly (AIA) onboard the Solar Dynamics Observatory molecular clouds to the Jovian moon Europa. There (SDO). QFPs are not uncommon and are generally have been various efforts to develop new techniques associated with some, but not all solar flares and/or to replicate these environments and study these ices coronal mass ejections (CMEs). To search for phys- in the laboratory. From an astrochemical point of ical conditions that can contribute to QFP produc- view, the development is key for understanding how tion, we carried out a systematic survey of QFPs from the energetic processing of ice can lead to molecu- the full SDO mission. We found that about 1/5 of lar complexity. From a planetary science point of global EUV waves were associated with QFPs. We view, the development is driven to investigate novel

75 also conducted a comparative study of two active 4 National Radio Astronomy Observatory (Charlottesville, Virginia, regions (ARs) visible between October and Novem- United States) ber 2014, AR12192 and AR12205, with very differ- ent levels of QFP activity. AR12205 produced less Solar termination shocks (TSs) can form above the flares but more QFPs, which were all associated with looptop when reconnection outflows that impinge blow-out, eruptive flares and global EUV waves. In upon newly reconnected flare arcades exceed the lo- contrast, AR12192 produced more (mostly confined) cal fast-mode magnetosonic speed. TSs have been flares, but with virtually no QFPs and less CMEs. suggested as one of the promising drivers for par- This suggests that blow-out eruptions could be a nec- ticle acceleration in solar flares, yet observational essary, but not sufficient condition for QFP produc- evidence remains rare. By utilizing radio dynamic tion and/or detectability. spectral imaging of decimetric stochastic spike bursts (SSBs) observed during a C1.9 eruptive flare on 2012 210.02 — Quasi-Periodic Pulsations Observed in March 3, Chen et al. (2015) found that the bursts were White Light at the Loop Top of the SOL2017-09-10 associated with a dynamic TS-like feature above the X8.2 Flare looptop. They also showed evidence for the TS as an electron accelerator. One piece of observational evi- Junwei Zhao1; Wei Liu1 dence that strongly supports the TS interpretation is 1 Stanford Univ. (Stanford, California, United States) the split-band feature – a phenomenon well-known in type II radio bursts associated with CME-driven An X8.2 flare occurred on September 10, 2017 near shocks, one interpretation for which attributes to ra- the Sun’s west limb. Simultaneously with the obser- dio emission from both the upstream and down- vations of the SDO/AIA’s multiple UV/EUV chan- stream side of the shock. We perform detailed spec- nels, the continuum intensity of the SDO/HMI also tral imaging analysis of the split-band feature in the observed the evolution of the post-flare loop above 2012 March 3 SSB event, and find evidence that sup- the solar limb. This gives us a rare opportunity to ports the shock upstream-downstream interpreta- analyze the post-flare loop in visible light, UV, and tion. We also report another SSB event observed dur- EUV channels. Quasi-periodic pulsations, with a ing an M8.4 eruptive flare on 2012 March 10, and period close to about 8 minutes, are found in all show that the radio centroids of the SSBs form a these channels during the rise of the loop top. We similar shock-surface-shaped structure to the earlier study the spatial and temporal relations of the pul- event, located above the reconnected flare arcades sations observed in different wavelengths, and find and below supra-arcade plasma downflows. that EUV pulsations occurred about 2-3 minutes ear- lier, and 2-6 Mm higher in altitude, than the pul- 210.04 — Joint GST and EOVSA Observation of an sations observed in UV and white light. While the M1.4 Flare on 2017 September 6 UV observations show many similarities in the pul- sations with the white light observations, the UV Yuqian Wei1; Bin Chen1; Sijie Yu1; Haimin Wang1 intensity decayed with the rise of the loop but the 1 New Jersey Institute of Technology (Newark, New Jersey, United white light intensity grew for about 20 more minutes. States) These observations help shed light on our under- standing of the magnetohydrodynamics of the flare’s We study an M1.4 class flare occurred shortly after loop-top, as well as the emission mechanism of the the X9.3-class flare on 2017 September 6 in NOAA ac- white light off the solar limb. tive region (AR) 12673. The flare was well observed by the Expanded Owens Valley Solar Array (EOVSA), 210.03 — Radio Spectroscopic Imaging of Solar the Goode Solar Telescope (GST) at the BBSO, Hin- Flare Termination Shocks: Split-band Feature and ode, and RHESSI. We find a partial eruption of a A Second Possible Event flux rope in GST H-α images during the flare, with coronal counterparts seen in SDO/AIA images. Mi- Bin Chen1; Yingjie Luo1; Sijie Yu1; Sam Krucker2; Kathy crowave spectral imaging observations from EOVSA Reeves3; Chengcai Shen3; Timothy S. Bastian4 provide unique measurements of the coronal mag- 1 Center for Solar-Terrestrial Research, New Jersey Institute of netic field and energy distribution of the nonthermal Technology (Newark, New Jersey, United States) electrons accelerated to mildly relativistic energies. 2 University of California, Berkeley (Berkeley, California, United We compare the location and morphology of the mi- States) crowave source with H-α, EUV, and X-ray data, and 3 Center for Astrophysics Harvard-Smithsonian (Cambridge, Mas- discuss implications for energy release and electron sachusetts, United States) acceleration in this flare.

76 211 — iPoster Plus VII: Stars & We are developing a small satellite mission concept, the X-ray Quantum Calorimeter satellite (XQCSat), Friends capable of performing high-resolution X-ray spec- troscopy of diffuse gas in the interstellar medium 211.01 — System Parameters for the Eclipsing within the Galaxy and the Galactic halo. The high o Binary Systems BD+11 3569 and HD 51082 spectral resolution (6 eV) of XQCSat enables unam- biguous measurement of the physical state of hot gas Wesley Ryle1; Kylie Anderson1; Kelsey Etherton1; Cristi from individual spectral lines, while its wide field of Farwick1; Sierra O’Bryan1; Terri Perrino1; Raymond view provides more than two orders of magnitude Whitehill1 improvement in the study of diffuse emission rela- 1 Thomas More University (Crestview Hills, Kentucky, United tive to the microcalorimeter flown on Hitomi. XQC- States) Sat will study stellar feedback, how energy from stars We present the results from a combined spectro- and supernovae affects the surrounding stellar and scopic and photometric in-depth study of the binary galactic environment and transports metal produced systems BD+11o3569 and HD 51082. Fits to Johnson in stars, providing insight to the evolution and struc- V , Cousins R and I photometry and radial velocities ture of galaxies. XQCSat will probe the distribution yield system parameters for each star in the binary and dynamics of hot gas in the halo of the Milky Way systems with uncertainties of less than 2%. Both sys- to determine how it is heated and whether it con- tems include intermediate mass stars for which pre- tributes significantly to the total mass of the Milky cise, direct measurements of mass, radii, and tem- Way. Key to XQCSat is development of a small- perature are lacking. These systems were initially se- satellite compatible cryostat and adiabatic demag- lected based on photometric measurements from the netization refrigerator capable of cooling the focal All Sky Automated Survey (ASAS), with subsequent plane detector array to 50 mK. Demonstration of that spectroscopic and dedicated photometric measure- capability will enable small satellite missions in other ments carried out by the authors. wavebands such as the far-infrared.

211.02 — Multi-messenger Search for Binary 212.02 — Dark Cosmology: Investigating Dark Neutron Star Mergers Matter and Exotic Physics using the Redshifted 21-cm Global Signal with the Dark Ages Alexander Harvey Nitz1; Alex Nielsen1; Collin Capano1 Polarimeter Pathfinder (DAPPER) 1 AEI Hannover (Hannover, Niedersachsen, Germany) Jack O. Burns1; Stuart Bale2; Richard F. Bradley3 The observation of the binary neutron star merger 1 Univ. of Colorado at Boulder (Boulder, Colorado, United States) GW170817 heralded the age of multi-messenger as- 2 University of California at Berkeley (Berkeley, California, United tronomy. We’ll discuss the joint observation of States) GW170817 and GRB 170817A and how combining 3 National Radio Astronomy Observatory (Charlottesville, Virginia, information from multiple channels can improve the United States) search for the most distant binary neutron star merg- ers. Finally, we’ll explore results from a multi- We report on the results of a NASA-funded As- messenger search using public LIGO and Fermi data. trophysics SmallSat concept study for a proposed lunar-orbiting experiment, the Dark Ages Polarime- ter PathfindER (DAPPER), that is designed toob- 212 — NASA Astrophysics Science serve the unexplored Dark Ages epoch of the early Universe. The Dark Ages, probed by the highly red- SmallSat Studies shifted 21-cm neutral hydrogen global signal, is the ideal epoch for a new rigorous test of the standard 212.01 — XQCSat - X-Ray Quantum Calorimeter LCDM cosmological model. DAPPER will search for Satellite divergences from the standard model that will in- Philip Kaaret1; Dan McCammon2; David Frank3; Toan dicate new physics such as heating or cooling pro- Nguyen4 duced by dark matter. A broad absorption trough 1 University of Iowa (Iowa City, Iowa, United States) in the redshifted 21-cm spectrum is expected during 2 University of Wisconsin (Madison, Wisconsin, United States) the Dark Ages, prior to the formation of the first stars 3 Lockheed Martin Space (Palo Alto, California, United States) and thus determined entirely by cosmological phe- 4 Blue Canyon Technologies, Inc. (Boulder, Colorado, United States) nomena. DAPPER will observe this pristine epoch

77 (17-38 MHz; z∼83-36), and will measure the am- and high cadence (95 minutes) will enable us to de- plitude of the 21-cm spectrum to the level required termine the origin of the early UV-bright emission to distinguish (at >5-σ) the standard cosmological from binary neutron star mergers - such observa- model from that of additional cooling derived from tions cannot be accomplished from the ground, due recent EDGES results. The main challenge of this to atmospheric transmission (bandpass) and visibil- measurement is the removal of bright foregrounds. ity constraints (cadence). DAPPER is designed to overcome this by utilizing While not following up binary neutron star merg- two pioneering techniques: (1) a polarimeter to mea- ers, GUCI will conduct the first synoptic survey of sure polarization induced by the anisotropic fore- the UV transient sky, imaging 1500 square degrees grounds and large antenna beam to aid in the separa- every 3 hours to a depth of 19.0 mag (AB). GUCI tran- tion of the foregrounds from the isotropic, unpolar- sient discoveries will address key Decadal Survey ized global signal, and (2) a pattern recognition anal- science questions such as how super-massive black ysis pipeline based on well-characterized training holes accrete material and influence their surround- sets of foregrounds from sky observations, instru- ings, and which massive stars give rise to the differ- ment systematics from simulations and laboratory ent classes of core-collapse supernovae. It will nat- measurements, and signals from theoretical predic- urally complement the Large Synoptic Survey Tele- tions. End-to-end simulations of the DAPPER instru- scope and Square Kilometer Array in these time- ment including thermal noise, systematics from the domain studies. spectrometer/polarimeter and the beam-averaged The key enabling technology for GUCI is the de- foreground, along with 21-cm models which in- velopment of delta-doped CCD detectors, providing clude added cooling meet our sensitivity require- an order-of-magnitude improvement in throughput ments to separate the standard cosmological mod- over the microchannel plates used for GALEX and els from ones that point toward new physics. DAP- the UVOT on Swift. Even with the modest aper- PER’s science instrument consists of dual orthog- ture required by a cubesat form factor, GUCI will onal dipole antennas and a tone-injection receiver achieve sufficient sensitivity to detect binary neutron based on high TRL components from the Parker star mergers out to at least 100 Mpc. Solar Probe/FIELDS, CURIE, and WIND/WAVES. In this talk we describe the scientific objectives, in- DAPPER will be deployed into a frozen 50x125 km strument and mission implementation for the GUCI lunar orbit to provide 4615 hours of radio-quiet inte- concept. gration over a 26 month lifetime. 212.04 — MASS (MicroArcsecond Small Satellite)

212.03 — The Gravitational-wave Ultraviolet 1 Counterpart Imager (GUCI) Network Michael Shao 1 JPL (Pasadena, California, United States) Stephen B. Cenko1 MASS is an ESPA class Mission that is one of the 1 NASA Goddard Space Flight Center (Greenbelt, Maryland, NASA funded AS3 studies. It uses with a 35cm aper- United States) ture and a large format CMOS sensor designed to The Gravitational-wave Ultraviolet Counterpart Im- achieve 4∼5 microarcsec astrometric precision in ∼ ager (GUCI) network is a SmallSat mission concept 1hr on bright nearby stars against ∼100 nearby refer- designed to identify and characterize the early (dt ence stars as bright as 10 mag within a ∼1/2 degree < 1 d) UV emission from binary neutron star merg- FOV. The scientific goal is to search for exoplanets ers. GUCI is comprised of 2 independently operat- down to 1 Earth mass around a ∼1/2 dozen of the ing 12U cubesats in low-Earth orbits, each equipped nearest stars and up to ∼20 stars down to 2 Earth with a wide-field (∼ 50 square degrees) UV imager. mass in the habitable zone. Transit searches favor We will promptly uplink sky localizations of binary planets with of days. This astromet- neutron star mergers from gravitational wave detec- ric search compliments the transit searches for exo- tors to the spacecrafts. Unlike ground-based optical Earths because astrometry is more sensitive to plan- observatories that suffer from visibility (e.g., wait- ets with oribital periods of ∼ 1 year around FGK ing for night to begin observing) and weather con- stars. This high precision is achieved through a laser straints, GUCI will begin imaging of gravitational calibration of the focal plane detector at the ∼1e-4 wave localizations within one hour (on average). pixel level, along with a highly stable thermal de- Each satellite will have a distinct bandpass, but will sign for both the telescope and focal plane, and a otherwise be identical. The multi-filter UV coverage diffractive pupil to measure the distortion of the op- tics. While technological advances allow such high

78 precision, another significant enabler for this type exoplanet hosts at an unprecedented level. This, in of mission is the dramatically lower cost of ESPA turn, will provide valuable constraints for models of Class spacecraft that are now becomming available atmospheric loss. and rather popular. ESPA class spacecraft with up to 250Kg mass 400W and sub-arcsec pointing stability 212.07 — The Virtual Telescope for X-ray have dramatically dropped in cost in the recent past Observations (VTXO) and enable very capable science missions for a frac- 1 tion of a SMEX or MIDEX. John Krizmanic 1 CRESST/NASA/GSFC/UMBC (Greenbelt, Maryland, United 212.05 — Placeholder: Bruce Macintosh States) 212.06 — SEEJ: Smallsat Exploration of the The Virtual Telescope for X-ray Observations (VTXO) Exospheres of Nearby Hot Jupiters will use lightweight Phase Frensel Lenses (PFLs) with near diffraction-limited performance in a vir- 1 Scott J. Wolk tual X-ray telescope with ∼1 km focal length 1 SAO (Cambridge, Massachusetts, United States) and with ∼50 milli-arcsecond angular resolution. While laboratory tests of PFLs have achieved near The first detected exoplanets found were “Hot diffraction-limited angular resolution in the X-ray Jupiters”; these are large Jupiter-like planets in close band, they require long focal lengths to achieve this orbits to their host star. The stars in these so-called quality of imaging. VTXO is formed by using preci- “ systems” can have significant X-ray sion formation flying of two SmallSats: a smaller Op- emission and the X-ray flux likely changes the evo- ticsCraft that houses the PFLs and a larger Detector- lution of the overall star-planetary system in at least Sat that contains an X-ray camera and propulsion for two ways: the formation flying. The baseline flight dynamics (1) the intense high energy flux alters the structure uses an elliptical orbit to allow the formation to hold of the upper atmosphere of the planet – in some cases in an inertial frame around perigee for an extended leading to significant mass loss; period. VTXO’s fine angular resolution enables mea- (2) the angular momentum and magnetic field of suring the environments closer to the central engines the planet induces even more activity on the star, en- in compact X-ray sources, allowing for the study of hancing its X-rays, which are then subsequently ab- the effects of dust scattering halos nearer to thecen- sorbed by the planet. tral objects in Cygnus X-3 and GX 5-1, the search for If the alignment of the systems is appropriate, the dust scattering echoes nearer to the central object in planet will transit the host star. The resulting drop X-ray transients, and the search for sub 0.1 arcsecond in flux from the star allows us to measure the distri- structures in the plerion nebula around the Crab pul- bution of the low density planetary atmosphere. sar and in the wind environments ambient to bright We describe a science mission concept for a Small- X-ray binaries such as Cyg X-1. The fine angular res- sat Exploration of the Exospheres of hot Jupiters olution could also potentially resolve structure in the (SEEJ; pronounced “siege”). SEEJ will monitor the X- enigmatic Gamma Cassiopeiae, resolve X-ray ray emission of nearby X-ray bright stars with transit- sources in regions of high stellar density, and allow ing hot Jupiters in order to measure the lowest den- for studying the effects of space weather on nearby sity portion of exoplanet atmospheres and the coro- exoplanets. The VTXO SmallSat and instrument de- nae of the exoplanet hosts. SEEJ will use revolu- signs, mission description, and science performance tionary Miniature X-ray Optics (MiXO) and CMOS will be described. X-ray detectors to obtain good collecting area and high sensitivity in a low mass, small volume and low- 212.08 — Concept Study for the HREXI SmallSat cost package. SEEJ will observe scores of transits PathfinderHSP ( ) Mission occurring on select systems to make detailed mea- surements of the transit depth and shape which can Jonathan Grindlay1; JaeSub Hong1; Branden Allen1; be compared to out-of-transit behavior of the target Daniel Violette1; Fiona Harrison2; scott barthelmy3; system. The depth and duration of the of the flux Benjamin Cervantes4; Marc Fouquet5 change will allow us to characterize the exospheres 1 Astronomy, Harvard University (Cambridge, Massachusetts, of multiple hot Jupiters in a single year. In addition, United States) the long baselines (covering multiple stellar rotation 2 Caltech (Pasadena, California, United States) periods) from the transit data will allow us to char- 3 NASA/GSFC (Greenbelt, Maryland, United States) acterize the temperature, flux and flare rates ofthe 4 NASA/WFF (Wallops, Virginia, United States)

79 5 Blue Canyon Technologies (Boulder, Colorado, United States) ISCEA (Infrared SmallSat for Cluster Evolution As- trophysics) is a small space mission that will study X-ray Time-domain Astrophysics (TDA) enables a the evolution of the Universe during the peak of wide range of high priority studies: from the birth galaxy formation. I will describe the ISCEA mission of stellar mass black holes (LGRBs) at high redshifts concept, and the findings of the NASA-funded con- to the tidal disruption of stars and production of rel- cept study. ativistic jets by dormant supermassive black holes in galaxies, to name a few. We describe our AS3 Con- cept Study for the High Resolution Energetic X-ray 213 — Laboratory Astrophysics Imager (HREXI) SmallSat Pathfinder (HSP) mission, a 3 –200 keV coded aperture telescope with a 36ox36o Division Meeting (LAD): Bridging FoV. HSP is a Pathfinder for a proposed future 4pi Laboratory & Astrophysics: X-ray Imaging Observatory (4piXIO), the first full- sky-continuous-imaging survey. HSP has 960 cm2of Molecules and Spitzer II imaging CdZnTe (CZT) detectors with 15-150 keV sensitivity similar to Swift/BAT plus 3-15 keV cov- 213.01 — LAD Early Career Award: GOTHAM erage not covered by BAT. The 4.6 arcmin resolution and ARKHAM: First Results from Programs to gives ≤28 arcsec source positions. HSP will survey Explore Aromatic Chemistry at the Earliest Stages the Galactic Bulge for flaring of quiescent BH-LMXBs of Star Formation and black hole candidates down to Lx(3-30 keV) =1.5 1,2 33 Brett A. McGuire x 10 erg/s, that of the BH-LMXB V404Cyg in qui- 1 National Radio Astronomy Observatory (Charlottesville, Virginia, escence. HSP will survey 2 nearby (0.5 kpc) OB as- United States) sociations for low-luminosity BHC-HMXBs accret- 2 Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- ing from weak-wind O8-9V stars, as sachusetts, United States) found with NuSTAR in the Carina OB2 association (Grindlay+2019, in prep). HSP would reach Lx(3- I will present an overview of the GOTHAM (GBT Ob- 30 30 keV) = 6 x 10 erg/s (∼15X lower than the NuS- servations of TMC-1: Hunting Aromatic Molecules) TAR candidate). Both the qBHC-LMXBs and BHC- and ARKHAM (A Rigorous K-band Hunt for Aro- HMXBs are recognized by their detection at ener- matic Molecules) projects on the 100 m Robert C. gies >10 keV. There should be ∼30X more weak-wind Byrd Green Bank Telescope, and a number of first BH-HMXBs than Cyg X-1 systems, the ratio of O results. These observations, prompted by our ear- star main sequence/super-giant lifetimes. The HSP lier detection of benzonitrile (c-C6H5CN) in TMC-1, compact coded aperture telescope mounts on a Blue are designed to probe the extent of hidden chemi- Canyon Technologies Microsat-S5 spacecraft which cal complexity at the earliest stages of the star for- provides ∼1 arcmin inertial pointing with continu- mation process. I will discuss the detections of ous ∼5arcsec aspect data from 2 star trackers. Two new molecules in TMC-1, comment on the prospects body-mounted solar panels deliver the 69 W instru- for probing additional aromatic chemistry in this ment/spacecraft power, and Xband patch antennas source, and examine the apparently widespread na- downlink prompt positions and fluxes for GRBs and ture of benzonitrile through the early protostellar transient alerts and full data (0.6GB/day) in sev- phase of star formation. These observations are be- eral NEN passes per day. The 96kg payload mass ing conducted in coordination with dedicated lab- is mounted within a standard ESPA volume for a oratory efforts to examine the formation routes of 표 Rideshare launch into a 25 –30 inclination, 600 km these species in the laboratory, and I will further LEO orbit. Positions and fluxes for all prompt GRBs discuss recent results concerning the formation of and Transients would be immediately available by benzene, benzonitrile, and related molecules using GCNs, followed by full light curves and spectra as chirped-pulse and cavity-enhanced microwave spec- they are processed and posted on the HSP mission troscopy. public web-site. 213.02 — Spitzer’s View of the Aromatic Universe 212.09 — ISCEA: Infrared SmallSat for Cluster Evolution Astrophysics Jan Cami1,2; Els Peeters1,2 1 The University of Western Ontario (London, Ontario, Canada) 1 Yun Wang 2 SETI Institute (Mountain View, California, United States) 1 California Institute of Technology (Pasadena, California, United States)

80 A significant fraction (∼15%) of the carbon in the structure and chemistry of a significant part of the Universe resides in large, aromatic molecules that dust grain population. Suggestions to date for the are widespread and ubiquitous in our Milky Way ERE carrier will be reviewed briefly. It is prominent and other galaxies. Through their molecular proper- in spectra of the Red Rectangle - a mixed-chemistry ties and sheer abundance, they control the tempera- object which comprises a HD 44179, a cir- ture of interstellar gas, and play key roles in radiative cumstellar disk and an extended carbon-rich bipo- feedback processes that directly influence large-scale lar nebula from which ERE is emitted. Given strong processes like star formation and galaxy evolution. infrared emission from PAHs in the nebula, it may In addition, they are driving important chemical pro- be suspected that aromatic carbon structures form cesses as well, including H2-formation. part of the key to identifying the ERE carrier. In this Much of the aromatic carbon is in the form of poly- study comparison between laboratory luminescence cyclic aromatic hydrocarbon species (PAHs) whose and astrophysical ERE spectra reveals that large aro- presence is revealed by a set of characteristic vibra- matic structures which include heteroatoms have tional features in the IR. However, not a single PAH spectral characteristics which are consistent with the species has been reliably identified in space, and our observed ERE feature. This proposal is supported by ignorance about the identity of the cosmic PAH fam- observation of complementary infrared bands in ISO ily hinders our progress in understanding and de- and Spitzer spectra of ERE-emitting objects. scribing these key processes in detail. On the other hand, fullerenes (and in particular C60) have been 213.04 — Formation of Interstellar C60 from identified and detected in a variety of astrophysical Silicon Carbide Circumstellar Grains environments – from the circumstellar carbon-rich 1 1 1 surroundings of evolved stars to interstellar reflec- Jacob Bernal ; Lucy M. Ziurys ; Pierre Haenecour ; Jane 2 1 3 tion nebulae and young stellar objects. Fullerenes Howe ; Thomas Zega ; Sachiko Amari 1 share many properties with PAHs, and are also often University of Arizona (Tucson, Arizona, United States) 2 found in environments where PAHs reside as well. University of Toronto (Toronto, Ontario, Canada) 3 Laboratory experiments as well as theoretical calcu- Washington University in St. Louis (St. Louis, Missouri, United lations and observational results furthermore sug- States) gest that fullerenes could well form from PAHs in The detection of C60 in astronomical sources has these environments. Understanding the specifics of changed our notions concerning the chemical com- how fullerenes form, evolve and respond to their en- plexity of the interstellar medium (ISM), and the vironment can thus provide important insights into repositories of gas-phase carbon. Furthermore, the astrochemistry and the characteristics of PAHs as + C60 cation has been proposed as a carrier of a few well. diffuse interstellar bands. Despite its ubiquitous In this talk, I will provide an overview of the un- presence, the mechanism of C60 formation remains precedented, detailed view that the Spitzer Space the subject of speculation. Several mechanisms have Telescope has offered us of the environments in been proposed, including destruction of polycyclic space where aromatics thrive and survive, and the aromatic hydrocarbons (PAHs). Here we propose a many new questions that surfaced as a result of it. new synthetic route to interstellar C60 from shock I will show how novel laboratory studies and - heating of SiC grains in the protoplanetary nebulae retical calculations have provided breakthrough in- phase. We have conducted laboratory experiments sights into the observational picture painted by the with analog SiC grains using techniques of transmis- Spitzer Space Telescope regarding the interstellar sion electron microscopy (TEM) and electron energy- physics and chemistry of PAHs and fullerenes. loss spectroscopy (EELS). The silicon carbide 3C polytype was used – the type commonly produced 213.03 — Extended Red Emission in the envelopes of AGB stars. We rapidly heated Peter J. Sarre1 small SiC crystals (∼ 50 nm) under vacuum to ∼ 1300 K thermally and with ion bombardment. TEM 1 School of Chemistry, The University of Nottingham (Nottingham, imaging and EELS spectroscopic mapping shows Nottinghamshire, United Kingdom) that such heating leaches silicon from the silicon car- Extended Red Emission (ERE) is a broad feature bide surface, creating layered graphitic sheets. Sur- which is commonly observed from UV-excited inter- face defects in the crystal were found to distort the stellar grains but its origin has not been established six-membered rings characteristic of graphite, creat- with certainty. A full assignment and understand- ing hemispherical structures with diameters match- ing of ERE would provide valuable insight into the ing that of C60. Such non-planar features require

81 the formation of 5-membered rings. We have sub- Boltzmann distribution, due to the presence of a re- sequently identified circumstellar grains, preserved cent merger referred to as the Gaia Sausage, leading inside primitive meteorites, that surprisingly con- to a weakening of direct detection limits at dark mat- tain a SiC core surrounded by graphite, contradicting ter masses less than 10 GeV. In an orthogonal study, long-standing thermodynamic predictions. The pro- we use Gaia DR2 to fit the local escape velocity of posed mechanism readily explains the presence of stars, and obtain the tail of the stellar velocity distri- C60 in proto-planetary (PPNe) and planetary nebu- bution that we compare to the full distribution previ- lae (PNe). Subsequent injection of C60, a chemically- ously found. We then study the differences between robust molecule, into the diffuse ISM from PNe ac- the two distributions which constrain the systematic counts for its presence in other interstellar sources. errors on the different methods.

214.03 — Dynamical evidence for a dark 214 — Cosmological Probes of substructure in the Milky Way halo Dark Matter III Ana Bonaca1; Adrian M. Price-Whelan2; David W. Hogg3; Charlie Conroy1; Nelson Caldwell1; Phillip 214.01 — Probing Dark Matter Particle Properties Cargile1; Benjamin D. Johnson1 with Ultra-High-Resolution CMB Lensing 1 Center for Astrophysics | Harvard & Smithsonian (Cambridge, Neelima Sehgal1,2 Massachusetts, United States) 2 1 Stony Brook University (Stony Brook, New York, United States) Princeton University (Princeton, New Jersey, United States) 3 2 Flatiron Institute (New York, New York, United States) New York University (New York, New York, United States)

I will discuss a novel and powerful way to probe Stars escaping globular clusters form thin, long and dark matter particle properties using deep, high- kinematically-cold tidal streams. In pristine condi- resolution cosmic microwave background (CMB) tions, these streams have nearly uniform density, gravitational lensing measurements. These mea- however, new Gaia observations of one such struc- surements can distinguish between cold dark mat- ture in the Milky Way halo have revealed a likely site ter and alternative dark matter models that can ex- of . The on-sky morphology suggests plain observational puzzles of small-scale structure. a recent, close encounter with a massive and dense I will also discuss a new experiment being devel- perturber. Known baryonic objects are unlikely per- oped, called CMB-HD, that can achieve this science turbers based on their orbital properties, but obser- and also open new windows on the early Universe, vations permit a low-mass dark-matter subhalo as gas and galaxy evolution, planetary studies, and the a plausible candidate. This observation opens up transient sky. the possibility that detailed observations of streams could measure the mass spectrum of dark-matter 214.02 — Empirical measurement of the local dark substructures and even identify individual substruc- matter velocity distribution and implications for tures and their orbits in the Milky Way halo. direct detection 214.04 — Testing Models of Dark Matter and 1 Lina Necib Modifications to Gravity using Local Milky Way 1 California Institute of Technology (Pasadena, California, United Observables States) Oren Slone1; Mariangela Lisanti1; Matthew Moschella1; Using two realizations of the Milky Way from the Nadav Outmezguine2 FIRE simulation, we find that the kinematics of dark 1 Physics, Princeton University (Princeton, New Jersey, United matter follows closely the kinematics of accreted States) stars from the same mergers. We use this correspon- 2 Tel Aviv University (Tel Aviv, Israel) dence to obtain an empirical measurement of the lo- cal velocity distribution of dark matter by analyzing Galactic rotation curves are often considered the first the Gaia second data release coupled with the ninth robust evidence for the existence of dark matter. release from the Sloan Digital Sky Survey, and com- However, even in the presence of a dark matter halo, puting the velocity distribution of the accreted stars. other galactic-scale observations, such as the Bary- We find that this velocity distribution is peaked at onic Tully-Fisher Relation and the Radial Accelera- lower velocities than the generally assumed Maxwell tion Relation, remain challenging to explain. This has motivated various models of dark matter but also

82 long-distance, infrared (IR) modifications to gravity For example, models that make use of the dissipa- as an alternative to the dark matter hypothesis, as tion of MHD turbulence to power the corona rely well as dark matter theories which reproduce phe- on lower boundary conditions in the photospheric nomenology similar to such modified gravity scenar- granulation. Using the Sun’s granular velocity field ios. We present a framework to test a general class for, say, the corona of an M dwarf would not be of such models using local Milky Way observables, appropriate. Also, using the output of convection- including the vertical acceleration field, the rotation driven wave-flux models to adjust the solar param- curve, the baryonic surface density, and the stellar eters to those of other stars may not be appropriate disk profile. In this talk I will focus on models that either. In the case of nearby M dwarf AU Mic, this predict scalar amplifications of gravity, i.e., models kind of extrapolation ended up drastically under- that increase the magnitude but do not change the predicting the amount of coronal heating observed direction of the gravitational acceleration. MOdi- in X-ray and submillimeter emission. It has been sus- fied Newtonian Dynamics (MOND) as well as Super- pected that – for the coronae of cool stars with dif- fluid dark matter are examples. We find that mod- ferent properties than the Sun – the most important els of this type are in tension with observations of wave/turbulence modes and dissipation channels the Milky Way scale radius and bulge mass and that may be fundamentally different from those most im- cold non-interacting dark matter provides a better portant in the solar atmosphere. Thus, conclusions fit to the data. We conclude that models that result from solar simulation codes about extrasolar wind in a MOND-like force struggle to simultaneously ex- mass loss rates, magnetospheres, and EUV/X-ray ir- plain both the rotational velocity and vertical motion radiances may need to be reevaluated with more ap- of nearby stars in the Milky Way. A future publica- propriate boundary conditions and coronal heating tion will extend this analysis to include other models physics. such as Self Interacting Dark Matter and dark matter with large baryon scattering cross sections. 215.02 — On the Formation of Wide Binary sdB and sdO Stars 215 — Stars & Stellar Topics II Lorne A. Nelson1; Abdel Senhadji1 1 Bishop’s Univ. (Sherbrooke, Quebec, Canada) 215.01 — Simulations of Stellar Winds and Exoplanet Magnetospheres: Hidden Assumptions We present a detailed analysis of the conditions re- in the Boundary Conditions quired to form stars in wide binaries via stable Roche Lobe overflow. Starting with an evo- 1 Steven R. Cranmer lutionary grid of almost 4000 primordial binaries 1 Astrophysical & Planetary Sciences, University of Colorado Boul- with component masses between approximately 1 der (Boulder, Colorado, United States) to 8 Msun and initial orbital periods of ∼1 to 200 days, many of these binaries experience an Algol-like For at least a century, the Sun has served as a use- phase of evolution and a substantial fraction of those ful template for our understanding of stellar atmo- produce binaries containing subdwarfs with orbital spheres. This is especially true for the observational periods of between ∼20 to 500 days. We conclude signatures of magnetic fields, hot coronae, and out- that: (1) the final period is largely dependent on the flowing winds, all of which have been tradition- assumed physics of non-conservative mass transfer; ally difficult to detect and characterize around other (2) the donor star (subdwarf progenitor) typically has stars. Recently, the solar community has developed a mass of between about 3 and 6 solar masses; (3) a number of self-consistent multidimensional simu- there is a very natural evolution of subdwarfs from lations of the Sun’s coronal heating and wind accel- a long-lived sdB stage (∼100 Myr) to the sdO stage eration, and these models have been quite success- (∼30 Myr); and, (4) the range of masses and effec- ful in reproducing a range of local measurements. tive temperatures of sdB and sdO stars can overlap These models are now being applied to other stars, substantially depending on the properties of the pri- with conclusions often being drawn from their out- mordial binary. Specifically we find that the masses put about the habitability of exoplanets circling those can range from ∼0.4 to 0.8 Msun, and that sdBs have stars (i.e., magnetospheric plasma conditions, mag- temperatures in the range of 15000 < T (K) < 45000 netic fields, and high-energy radiation). However, eff while the range for sdOs is about 25000 < Teff (K) there are sometimes subtle parameters embedded in < 100000. One example of a post-Algol binary that these models that have been fine-tuned for the Sun is evolving towards the subdwarf stage is MWC882 and not varied when applying them to other stars.

83 (Zhou et al. 2018). The observational implications of spiral-arm pitch angle; (v) central velocity disper- this channel are also discussed. sion; (vi) maximum disk rotational velocity, and in turn, (vii) dark matter halo mass. Notably, we 215.03 — High resolution imaging of red find separately for spiral galaxies (Sp) and early-type supergiants: A long-term imaging project with the galaxies with a disk (ES/S0) and without a disk (E), CHARA Array that log(MBH) ∝ 2log(M∗,푏푢푙푔푒). Furthermore, the three subsamples have different MBH/M∗,푏푢푙푔푒 ra- 1 1 Ryan P. Norris ; Fabien Baron 10 1 tios. At M∗,푏푢푙푔푒 = 5 × 10 M⊙,MBH/M∗,푏푢푙푔푒 = 2%, Georgia State University (Atlanta, Georgia, United States) 1%, and 0.1%, for ES/S0, Sp, and E galaxies, re- spectively. Similarly, log(M ) ∝ 2log(M ) for Convection plays an important role in the transport BH ∗,푔푎푙푎푥푦 early-type galaxies, while late-type galaxies exhibit of material within many stars. In stars like the sun, a steeper relation with log(M ) ∝ 3log(M ). the size of convection-related surface features is a BH ∗,푔푎푙푎푥푦 These results pose important benchmarks for forma- small percentage of the surface radius. However, tion theories and simulations, representing a signifi- in red supergiants (RSGs), granules and convection cant departure from the widely adopted “linear” re- cells are much larger. Understanding surface fea- lation traditionally applied to all morphologies with tures on RSGs–particularly their size, contrast, and the same M /M ratio. lifetime–is vital to understanding these stars in a BH ∗,푏푢푙푔푒 more general sense. We present the results of a long-term study of surface features on RSG using 215.05 — Improving Binary Millisecond Pulsar the Michigan InfraRed Combiner (MIRC/MIRCx af- Distances with Gaia ter 2016) at the Center for High Angular Resolution Chiara M. F. Mingarelli1; Lauren Anderson1; Megan (CHARA) Array on Mt. Wilson. In the form of some Bedell1; David N. Spergel1,2 the highest resolution images of any star (apart from 1 Center for Computational Astrophysics, Flatiron Institute (New the Sun) yet produced, we present yearly surface im- York, New York, United States) ages spanning 2011-2012 and 2014-2016 for the star 2 Princeton University (Princeton, New Jersey, United States) AZ Cyg and images from 2015-2016 for SU Per. We analyze the size, contrast, and lifetime of the features, Improved distance measurements to millisecond providing a stringent test against 3-dimensional ra- pulsars can enhance pulsar timing array (PTA) sensi- diative hydrodynamics (3D RHD) models of RSGs. tivity to gravitational-waves, improve tests of general We also highlight future directions for research in relativity with binary pulsars, and more. Here we RSG surface imaging, including the impact of opti- report parallax-based distance measurements to six cal interferometers planned for construction during Gaia DR2 objects associated with International PTA the 2020-2030 decade. pulsars J0437-4715, J1012+5307, J1024-0719, J1732- 5049, J1910+1256, and J1843-1113. By multiplying 215.04 — Black Hole Mass Scaling Relations the posteriors of the PTA distances with the Gaia

1,2 2 distance to the companion, we improve the distance Benjamin L. Davis ; Alister Graham ; Nandini measurements, and provide a tentative detection of Sahu1,2; Ewan Cameron3 1 a previously unknown binary companion to J1843- Australian Research Council Centre of Excellence for Gravita- 1113. tional Wave Discovery (Hawthorn, Victoria, Australia) 2 Centre for Astrophysics and Supercomputing, Swinburne Univer- 215.06 — Depth and Mass of a Neutron Star Crust sity of Technology (Hawthorn, Victoria, Australia) 3 Oxford Big Data Institute, University of Oxford (Oxford, United Lauren Balliet1; William Newton1; Farrukh Fattoyev2 Kingdom) 1 Physics & Astronomy, Texas A&M University-Commerce (Com- merce, Texas, United States) We have performed multi-component photometric 2 Manhattan College (Riverdale, New York, United States) decompositions for the largest to date sample of 132 galaxies with dynamically measured supermas- Neutron stars are a valuable asset to modern nu- sive black hole masses. For the 48 late-type galax- clear astrophysics in that they provide a unique envi- ies, we have additionally measured their spiral-arm ronment to study matter under extreme conditions. pitch angle geometries and derived dark matter halo Much of the observational data obtained from neu- masses via their rotational velocities. We have inves- tron stars contains information about the structure tigated how black hole mass (MBH) correlates with and dynamics of the crust. Using such observations (i) bulge, (ii) disk, and (iii) galaxy stellar mass; (iv) to measure crust properties requires understanding

84 the uncertainty range from models of the thickness 1 Washington University in St. Louis (St. Louis, Missouri, United of the different layers of the crust. These uncertain- States) ties arise from uncertainties in the properties of nu- 2 Hiroshima University (Hiroshima, Japan) clear matter. I will use a comprehensive ensemble 3 University of New Hampshire (Durham, New Hampshire, United of nuclear matter equations of state, spanning the States) current uncertainty in the nuclear interaction, to ex- 4 Stony Brook University (Stony Brook, New York, United States) amine the correlations between the crust thickness, 5 NASA’s Wallops Flight Facility (Wallops Island, Virginia, United mass distribution, and nuclear matter parameters. States) I will compare the results of a number of different 6 Guarino Engineering (Oak Park, Illinois, United States) ways to calculate the crust thickness and mass dis- 7 KTH (Stockholm, Sweden) tribution, and use them to estimate the uncertainty 8 RIKEN (Wako, Japan) in estimates of crust oscillation frequencies and the 9 Brookhaven National Lab (Upton, New York, United States) crust cooling time. 10 NASA’s Goddard Space Flight Center (Greenbelt, Maryland, United States) 215.07 — The Heating and Cooling of Neutron Stars X-ray polarimetry promises geometrical information about compact astrophysical objects such as accret- Brianna Douglas1; William Newton1 ing black holes and neutron stars that are too small 1 Physics and Astronomy, Texas A&M University - Commerce to be imaged at any wavelength. While some infor- (Commerce, Texas, United States) mation about the source geometry can be derived from spectral and timing measurements of the high- Information about the structure and evolution of energy emission, results are often model dependent. stars can be obtained from modeling their X-ray polarimetry can break these degeneracies by thermal evolution. I will present two studies, one of providing two new observables, namely the Stokes the cooling the Crab pulsar, and one of the heating parameters Q and U. X-Calibur is a balloon-borne of accreting neutron stars as they accrete matter from hard X-ray polarimeter covering the 20-40keV energy a companion star. Firstly, there is some circumstan- range. It consists of an 8m long optical bench car- tial evidence that the Crab pulsar was formed in an rying the InFOCμS hard X-ray mirror, and a scat- electron-capture supernova, which is one way stars tering polarimeter at its focal point. The optical about 8-10 solar masses die. In this type of super- bench is pointed with arc-second precision by the nova, the star’s core collapses at the ONeMg stage, Wallops Arc-Second Pointer (WASP). The polarime- and produces a relatively low mass neutron star of ter consists of a Beryllium scattering element at the around 1.25 solar masses. I calculate the cooling of focal point of the mirror surrounded by CZT detec- low mass neutron stars and compare with measured tors on 4 sides to measure azimuthal scattering angle upper limits on the Crab’s temperature. Secondly, and energy of the scattered photons. X-Calibur was I consistently model the accretion of matter onto a flown on a 2.5 day long stratospheric balloon flight population of neutron stars and the subsequent heat- from McMurdo (Antarctica) from Dec. 29, 2018 to ing caused by nuclear reactions as the accreted mat- Jan. 1, 2019. The observations caught the accreting X- ter is buried. The distribution of crustal heating as a ray pulsar GX 301-2 close to the apastron at elevated function of initial period, magnetic field, and equa- flux levels. We report here on the first X-Calibur re- tion of state is presented. sults including the 15-60 keV light curve, the hard X- ray energy spectrum, and the first constraints on the 215.08 — Results From the Antarctic Balloon polarization of the hard X-ray emission. We further- Flight of the Hard X-ray Polarimeter X-Calibur more show results from simultaneous observations with the Neil Gehrels Swift and NICER X-ray tele- Fabian Kislat2; Quincy Abarr1; Richard Bose1; Dana 1 3 1 scopes. We conclude with an outlook of the physi- Braun ; Gianluigi de Geronimo ; Paul Dowkontt ; cal constraints that can be derived based on future, Manel Errando1; Thomas A. Gadson4; Victor Guarino5; 4 6 6 deeper X-ray spectropolarimetric observations of X- Scott E. Heatwole ; Nirmal Iyer ; Mózsi Kiss ; Takao ray pulsars. Kitaguchi7; Henric Krawczynski1; Rakhee Kushwah6; James Lanzi4; Shaorui Li8; Lindsey Lisalda1; Takashi Okajima9; Mark Pearce6; Zachary Peterson4; Brian Rauch1; David Stuchlik4; Hiromitsu Takahashi10; Jason Tang1; Nagomi Uchida10; Andrew West1

85 216 — Solar Physics Division 216.02 — Magnetic Energy Release in Solar Flares seen through Microwave Eyes Meeting (SPD), Flares I Gregory D. Fleishman1; Dale E. Gary1; Bin Chen1; Sijie 216.01 — Fast plasma outflows associated with Yu1; Gelu M. Nita1; Natsuha Kuroda1 impulsive microwave and hard X-ray bursts 1 NJIT (Newark, New Jersey, United States) during the gradual phase of the 2017 September 10 X8.2 flare Solar Coronal Magnetism includes emergence of the magnetic flux from the sub-photospheric volume, Bin Chen1; Sijie Yu1; Sophie Musset2; Dale E. Gary1; evolution of the coronal magnetic field, generation Gregory D. Fleishman1; Lindsay Glesener2; Kathy and accumulation of a free non-potential magnetic Reeves3; Gelu M. Nita1 energy, gradual and explosive release of this energy, 1 Center for Solar-Terrestrial Research, New Jersey Institute of generation and dissipation of turbulence. This set Technology (Newark, New Jersey, United States) of phenomena drives solar flares and other forms of 2 University of Minnesota (Minneapolis, Minnesota, United States) eruptive activity such as jets or coronal mass ejec- 3 Center for Astrophysics Harvard-Smithsonian (Cambridge, Mas- tions. An emerging new remote sensing window— sachusetts, United States) Microwave Imaging Spectroscopy—offers a science- transforming, entirely new look at the coronal mag- The 2017 September 10 X8.2 flare is a spectacular netism. The foundation of this new capability is long duration event associated with a fast coronal the sensitivity of the microwave emission to the mass ejection (CME). It features an extended grad- magnetic field. A break-through, however, comes ual phase associated with hard X-ray (HXR) and only when this emission is measured at many fre- microwave (MW) bursts that last for at least two quencies with a reasonably high spatial and tem- hours after the flare peak (at ∼1600 UT). We exam- poral resolution, which is the case of a new imag- ine the gradual phase using multi-wavelength data ing instrument—the Expanded Owens Valley Solar recorded by the Expanded Owens Valley Solar Ar- Array (EOVSA). In this talk we briefly present the ray (EOVSA), RHESSI, Fermi/GBM, SDO/AIA, and key methodology needed to obtain the target physi- MLSO/K-Cor. During the extended gradual phase cal parameters, show a few examples of solar flares (∼17-18 UT) when the CME already propagates to observed with EOVSA, and discuss main physical >10 solar radii, an extremely long and thin plasma findings made with these new data and methodol- sheet is visible in white light (WL) images that ex- ogy, in particular—about rapid decay of the mag- tends to at least ∼1.5 solar radii above the solar sur- netic field at the site of the primary energy release face. We find evidence of multitudes of fast bi- in solar flares, associated electric field and acceler- directional plasma outflows (∼300-700 km/s) within ated particles, plasma heating, and turbulent mag- the plasma sheet emanating from localized sites at netic diffusivity. We discuss these new findings in very low coronal heights (0.1-0.2 solar radii above the context of the standard model of solar flare and the surface), interpreted as magnetic reconnection the contemporary ideas about the magnetic energy occurring in the low corona. The occurrence of the release, magnetic reconnection, turbulence genera- fast plasma outflows correlates very well in time with tion, and particle acceleration. the intermittent broadband MW emission and HXR enhancements. MW spectroscopic imaging reveals 216.03 — The Influence of Current Sheet Structure a MW source located at the looptop that coincides on Flare Loop Dynamics with a HXR looptop source. Another MW source is present in the northern leg of the flare arcade, whose John E. Unverferth1; Dana Longcope1 temporal evolution seems to correlate with the loop- 1 Department of Physics, Montana State University (Bozeman, top MW source but shows a time lag characteristic Montana, United States) of the Alfvén transit time. We examine the tempo- ral and spatial correlations among the plasma out- Solar flares are believed to result from magnetic re- flows, looptop MW/HXR source, and loopleg MW connection occurring within a coronal current sheet. source, and discuss implications for magnetic en- Flare energy is released as flux retracts through the ergy release, plasma heating, and electron accelera- sheet following its reconnection. This process is dic- tion during the extended gradual phase of the flare. tated by the magnetic field strength along the sheet through which the flux retracts. Some theoretical models, including the standard Petschek model, as- sume the field strength to be uniform along the sheet.

86 Others invoke a sheet terminating in field-free Y- reach their highest temperatures at the end of their points, so the field strength decreases steadily during retraction, well below the site of reconnection. Previ- retraction. Still others, including models of a collaps- ous analysis of AIA and EIS data had revealed a peak ing trap, assume the field strength increases as flux in the plasma temperature very near the base of this retracts. Each of these assumed configurations will particular sheet. This is consistent with our hypothe- lead to an observably different solar flare. We study sis that downflows descend from a higher reconnec- the effects of these different configurations using the tion point. thin flux tube (TFT) model of magnetic flux retrac- This work supported by grants from NASA/HSR tion following reconnection. This model has been and NSF/REU shown to yield Petschek-like results when a uniform current sheet is assumed. We modify the model to 216.05 — Structure and dynamics of the hot flaring study the effects of different current sheet configu- loop-top source observed by Hinode, SDO, rations. This allows us to compare flares set in cur- RHESSI, and STEREO rent sheets with both increasing and decreasing field 1 2 3 strength profiles. Kyoung-Sun Lee ; Hirohisa Hara ; Kyoko Watanabe ; 2 4 5 This work was supported by NASA’s HSR pro- Anand D. Joshi ; Shinsuke Imada ; David H. Brooks ; 6 7 8 gram. Phillip Dang ; Toshifumi Shimizu ; Sabrina Savage 1 CSPAR, The University of Alabama in Huntsville (Huntsville, 216.04 — Evidence for downflows in the narrow Alabama, United States) 2 plasma sheet of 10 Sep 2017, and their significance National Astronomical of Japan (Tokyo, Japan) 3 for flare reconnection National Defense Academy (Yokohska, Japan) 4 Nagoya University (Nagoya, Japan) Dana Longcope1; John E. Unverferth1; Courtney Klein1; 5 George Mason University (Fairfax, Virginia, United States) Marika McCarthy1; Eric R. Priest2 6 Software Developer at Call Box (Dallas, Texas, United States) 1 Montana State Univ. (Bozeman, Montana, United States) 7 ISAS/JAXA (Sagamihara, Japan) 2 Mathematics, University of St. Andrews (St. Andrews, United 8 MSFC/NASA (Huntsville, Alabama, United States) Kingdom) We have investigated an M1.3 flare on 2014 January Current sheets are believed to form in the wakes of 13 around 21:48 UT observed at the west limb us- erupting flux ropes and to enable the magnetic re- ing the Hinode, SDO, RHESSI, and STEREO. Espe- connection responsible for an associated flare. Multi- cially, the Hinode/EIS scanned the flaring loop cov- wavelength observations of an eruption on 10 Sep ering the loop-top region over the limb, which is a 2017 show a long, linear feature widely taken as ev- good target to investigate the dynamics of the flaring idence of a current sheet viewed edge-on. The re- loop with their height. Using the multi-wavelength lation between the high-temperature, high-density observations from the Hinode/EIS and SDO/AIA, plasma thus observed and any current sheet is not we found a very hot emission above the loop-top ob- yet entirely clear. We estimate the magnetic field served in Fe XXIV and 131Å channel. Measuring strength surrounding the sheet, and from that con- the intensity, Doppler velocity and line width for the clude that approximately one-third of all flux in the flaring loop, we found that hot emission observed active region was opened by the eruption. Sub- at the cusp-like shape of the loop-top region which sequently decreasing field strength suggests that shows strong redshift about 500 km s−1 in Doppler the open flux closed down over the next several velocity and strong enhancement of the non-thermal hours through reconnection at a rate dΦ/dt = 5 17 velocity (line width enhancement) larger than 100 × 10 Mx/s. We find in AIA observations evi- km s−1. Combining with the STEREO observation, dence of downward moving, dark structures anal- we have examined the 3D structure with loop tilt an- ogous to either supra-arcade downflows more typ- gle and have investigated the velocity distribution ically observed above flare arcades viewed face-on, of the loop-top region. With the loop tilt angle, we or to supra-arcade downflowing loops, previously could identify the strong redshift at the loop-top re- reported in flares viewed in this perspective. This gion may indicate an up-flow along the loop-top re- suggests that the plasma sheet is composed of the gion. From RHESSI hard X-ray (HXR), and soft X-ray magnetic flux retracting after being reconnected high (SXR) emission, we found that the footpoint bright- above the arcade. We use a model of flux tube retrac- ening region at the beginning of the flare has a both tion following reconnection to show that this process HXR (25-50 keV) and SXR (12-25 keV) emission in can generate high densities and temperatures as ob- which imply that the region has non-thermal emis- served in the plasma sheet. The retracting flux tubes

87 sion or accelerated particles. Then, within 10 min- might result in the obtained relationships between utes the soft X-ray (SXR) emission observed near the these gamma-ray components. cusp shape region at loop top. The temporal varia- tion of the HXR and SXR emissions and the Doppler velocity variation of the hot plasma component at the 217 — Solar Physics Division loop-top imply that the strong flow in a hot compo- Meeting (SPD), nent near loop-top could be the evaporation flows which detected at the corona along the tilted loop. Photosphere/Chromsphere Moreover, The temporal evolution of the tempera- ture observed by SDO/AIA and Hinode/EIS also 217.01 — GST high-resolution observations of shows the cooling process of the flare plasma which small-scale flux emergence in multiwavelengths is consistent with the impulsively heated flare model. Jiasheng Wang1; Chang Liu1; Haimin Wang1 1 Physics, New Jersey Institute of Technology (Newark, New Jersey, 216.06 — Gamma-ray emission from the impulsive United States) phase of the 2017 September 06 X9.3 flare The near-infrared imaging spectropolarimeter Alexandra L. Lysenko1; Sergey A. Anfinogentov2; (NIRIS) of the 1.6 m Goode Solar Telescope (GST) at Gregory D. Fleishman3; Dmitry S. Svinkin1; Dmitry Big Bear Solar Observatory (BBSO) produces vector Frederiks1 magnetograms at 0.24” resolution and up to 30 s 1 Ioffe institute (Saint Petersburg, Russian Federation) cadence. These unprecedented high spatiotemporal 2 Institute of Solar-Terrestrial Physics (ISZF) (Irkutsk, Russian resolution data provide us a unique opportunity to Federation) study the small-scale magnetic flux emergence and 3 New Jersey Institute of Technology (Newark, New Jersey, United cancellation events, which can advance our under- States) standing of the structural evolution of photospheric We report hard X-ray and gamma-ray observations fields and related dynamic activities spanning of the impulsive phase of the SOL2017-09-06T11:55 the solar atmosphere. In our previous study us- X9.3 solar flare. We focus on a high-energy part of ing NIRIS observations, we detected that during the spectrum, > 100 keV, and perform time resolved flux emergence there appears two components spectral analysis for a portion of the impulsive phase, of magnetic fluxes, the central diffused magnetic recorded by the Konus-Wind experiment, that dis- structure with enhancing horizontal field and con- played prominent gamma-ray emission. Given a va- centrated opposite-polarity fluxes at the two ends. riety of possible emission components contributing In this work, we jointly analyze NIRIS and other to the gamma-ray emission, we employ a Bayesian BBSO/GST observations of NOAA AR 12665 on inference to build the most probable fitting model. 2017 July 13, with the goal of shedding light on the The analysis confidently revealed contributions from signatures and responses of small-scale flux emer- nuclear deexcitation lines, electron-positron annihi- gence in multiple heights. We focus on case studies lation line at 511 keV, and a neutron capture line of flux emergence events near the magnetic polarity at 2.223 MeV along with two components of the inversion line. With direct imaging in broadband bremsstrahlung continuum. The revealed time evo- TiO (a proxy for continuum in photosphere at 705.7 lution of the spectral components is particularly in- nm) at 0.1” resolution and 15 s cadence, we observe teresting. The low-energy bremsstrahlung contin- that magnetic flux emergence is associated with uum shows a soft-hard-soft pattern typical for im- darkening of granular boundaries and elongation of pulsive flares, while the high-energy one shows a granules. When newly emerged magnetic elements persistent hardening at the course of the flare. The cancel with the existing opposite-polarity fields, neutron capture line emission shows an unusually bright point features are seen and they travel along short time delay relative to the nuclear deexcitation the intergranular dark lanes at a speed of about 4 line component, which implies that the production km/s. The canceled flux is in the order of 4x1016 Mx. of neutrons was significantly reduced soon after the In Hα observations (0.1 resolution and 34 s cadence) event onset. This may be caused by a prominent soft- at several line positions (±1.0, ±0.6, ±0.4, and line ening of the accelerated proton spectrum during the center), we see transient brightenings in the red flare, similar to the observed softening of the low- and blue wings, which are most probably Ellerman energy component of the accelerated electrons re- bombs. In a particularly well observed event, we sponsible for the low-energy bremsstrahlung contin- find brightenings in Hα red-wing(0.4 Å) around the uum. We discuss possible physical scenarios, which central diffused emerging region, where horizontal

88 flux density increases and peaks at 250 Mx/cm2; erates a series of slow mode shocks localized near when it restores to its initial state, the horizontal flux the null’s separatrices, leading to localized current density increases at the concentrated flux regions at densities and heating near each separatrix. We iden- the two ends. In the mean time, brightenings are tify the cause of the shocks and the current sheets also observed at concentrated flux footpoints in Hα and determine their dependence on the atmospheric far red-wing (0.6 Å, 1.0 Å). We suggest that these and wave packet parameters. We discuss the rela- observations may reflect the reconnection process tion between reconnection at the null, dissipation of between the emerging flux and overlying field. the shocks and current sheets, and the heating of features with similar magnetic topologies, such as 217.02 — On the Challenges of synthetizing solar coronal bright points. Using current estimates of the and stellar spectra for Irradiance reconstructions photospheric acoustic power, we estimate that the shock and Ohmic heating we describe may account Serena Criscuoli1; Matthias D. Rempel2; Margit for ∼1–10% of the radiative losses from X–ray and Haberreiter3; Tiago Pereira4; Han Uitenbroek1; Damian EUV bright points with similar topologies, and are Fabbian5 similarly insufficient to account for losses from larger 1 National Solar Observatory (Boulder, Colorado, United States) structures such as ephemeral regions. At the same 2 HAO (Boulder, Colorado, United States) time, the dynamics are comparable to recently pro- 3 PMOD (Davos, Switzerland) posed mechanisms for generating type–II spicules. 4 University of Oslo (Oslo, Norway) 5 University of Goettingen (Goettingen, Germany) 217.04 — ALMA detection of dark chromospheric holes Syntheses of solar and stellar spectra strongly de- pend on the adopted approximations and atomic and Stephen M. White1; Maria A. Loukitcheva2; Sami K. molecular databases. We compare LTE and NLTE Solanki2 syntheses of solar spectra obtained with widely used 1 Air Force Research Laboratory (Albuquerque, New Mexico, radiative transfer codes, utilizing both 3D-MHD sim- United States) ulations and 1D-static atmosphere models. We show 2 Max Planck Institute for Solar System Research (Goettingen, that although different codes reproduce reasonably Germany) well the observed spectrum, subtle differences may translate into discrepancies of several tens of per- Atacama Large Millimeter/submillimeter Array cents in the estimate of solar and stellar spectral ir- (ALMA) observations of a quiet-Sun region at a radiance variability. wavelength of 3 mm are compared with available chromospheric observations in the UV and visible 217.03 — The formation and dissipation of current as well as with photospheric magnetograms. The sheets and shocks due to compressive waves in a ALMA images clearly reveal the presence of dis- stratified atmosphere containing a magnetic null tinctive cold areas in the millimeter maps having temperatures of around 60% of the normal quiet Sun Lucas A. Tarr2; Mark Linton1 at 3 mm, which are not seen in the other data. We 1 Space Science Division, Naval Research Lab (Washington, Dis- speculate that ALMA is sensing cool chromospheric trict of Columbia, United States) gas, whose presence had earlier been inferred from 2 Physics and Astronomy, George Mason University (Fairfax, Vir- infrared CO spectra. ginia, United States) 217.05 — Shock heating energy in an umbra of a We study the propagation and dissipation of magne- sunspot with integral field unit spectroscopy tohydrodynamic waves in a set of numerical models that each include a solar–like stratified atmosphere Tetsu Anan1; Thomas A. Schad1; Sarah A. Jaeggli1; Lu- and a magnetic field with a null point. All simu- cas A. Tarr2 lations have the same magnetic field configuration 1 National Solar Observatory (Makawao, Hawaii, United States) but different heights for the model transition region, 2 George Mason University (Fairfax, Virginia, United States) where the temperature rapidly increases from pho- tospheric to coronal levels. Compressive wave pack- On 2014 December 7 we used new integral field ets introduced in the photospheric portion of the spectroscopy techniques to observe umbral flashes, simulations refract towards the null and collapse it which are periodic brightness increases routinely ob- into a current sheet, which then undergoes recon- served in the core of chromospheric lines within nection. Wave mode conversion near the null gen- sunspot umbrae and are attributed to propagating

89 shock fronts. In this work we quantify the shock 218 — Plenary Lecture: The Tools heating energy of these umbral flashes using ob- servations in the near infrared HeI triplet obtained of Precision Measurements in with the SpectroPolarimetric Imager for the Ener- Exoplanet Discovery and getic Sun (SPIES), which is novel integral field unit spectrograph at the Dunn Solar Telescope. We de- Characterization: Peeking under termine the shock properties (the Mach number and the Hood of the Instruments, the propagation speed) by fitting the measured HeI spectral profiles with a theoretical radiative trans- Suvrath Mahadevan (Pennsylvania fer model using two constant property atmospheric State University) slabs whose temperatures and macroscopic veloci- ties are constrained by the Rankine-Hugoniot rela- 218.01 — The Tools of Precision Measurements in tions. From the Mach number, the shock heating en- Exoplanet Discovery and Characterization: 10 ergy per unit mass of plasma is derived as 2 x 10 Peeking under the Hood of the Instruments erg/g. We conclude that the estimated shock heat- ing energy rate is less than the amount required to Suvrath Mahadevan1 maintain the umbral chromosphere. 1 Penn State (University Park, Pennsylvania, United States)

Modern astronomical instruments are approaching 217.06 — Counter-streaming motions in active the exquisite sensitivity to detect the signature of an region magnetic arches observed by Helium I Earth-mass planet around a Sun-like star. In this 10830Å spectroscopy talk I shall discuss the challenges involved in making Xu Yang1; Wang Ya2; Haisheng Ji2; Wenda Cao1 these difficult measurements with the Doppler radial 1 Physics, New Jersey Institute of Technology (Big Bear City, Cali- velocity technique, and the evolution of the design fornia, United States) of these instruments as they seek ever-tighter con- 2 Purple Mountain Observatory (Nanjing, China) trol of environmental parameters, higher resolution and efficiency, and to observe large spectral regions We report the first high-resolution observations of in the optical and infra-red. A suite of new tech- counter-streaming motions in the active region mag- nologies like frequency stabilized laser combs, low netic arches with Helium I 10830 Å spectroscopy, drift etalons, and deeper understanding of the de- achieved by the Goode Solar Telescope at Big Bear tectors is enabling a new level of precision in radial Solar Observatory. Our observations reveal that the velocity measurements – as well as illustrating new counter-streaming motions are due to unidirectional challenges. I will also describe how beam-shaping mass flows along alternative arches, rather than the diffusers are now enabling space-quality photome- longitudinal oscillations of filament threads as in try from the ground to aid in photometric follow-up some solar filaments. Mass flow, rooting in the and confirmation of transiting exoplanets. magnetic network region, are pumped up from and down to the inter-granulation lanes. The apparent speed of the flow is around 15-50 kms−1 in the He I 221 — Laboratory Astrophysics 10830 Å blue wing and 5-15 km s−1 in the red wing. Division Meeting (LAD): Bridging Co-spatial brightenings in Atmospheric Imaging As- Laboratory and Astrophysics: sembly 304 Å and 171 Å images are witnessed at the same time, indicating the possible corresponding Exoplanets II heating process. The oscillation power peaks around 4 minutes in the roots region of the arches, however, 221.01 — Studying exoplanet atmospheres with the mass flows inside the long arches seem to becon- laboratory data tinuous. Renyu Hu1 1 Jet Propulsion Laboratory (Pasadena, California, United States)

Observations of exoplanet atmospheres enable us to characterize their chemical composition, ther- mal structure, and general circulation. The ob- servations of atmospheric transmission and emis- sion via transit have been used to derive molecular

90 abundances, and this method works best for high- 221.03 — The Capabilities of LUVOIR for Studies temperature gaseous planets with H2-dominated at- of Exoplanet Diversity mospheres. Interpreting the transit observations de- Mark S. Marley1; Courtney Dressing2 pends on molecular and collision-induced opacities 1 in the relevant conditions, as well as an understand- NASA Ames Research Center (Moffett Field, California, United States) ing of whether photochemical hazes like those found 2 in the outer Solar System could form and survive UC Berkeley (Berkeley, California, United States) the high temperatures. Meanwhile, high-resolution, One of the great strengths of the proposed LUVOIR line-resolving spectroscopy using large ground tele- space observatory is that in addition to searching for scopes is a new avenue to detect molecules in exo- potentially habitable terrestrial planets, it will find planet atmospheres. This method relies on molec- and characterize hundreds of other types of plan- ular line lists with accurate wavelength positions. ets as well. This large population of planets will of- As the exoplanet field is planning future facilities fer unparalleled opportunities for comparative plan- and observations to characterize potentially habit- etary science over a wide range of masses, radii, able planets, new reaction rate constants, ultraviolet and orbital separations. Direct imaging and spec- cross sections, and molecular spectra (e.g., CH line 4 troscopy with ECLIPS, an ultra-high contrast coro- lists in the visible wavelengths and infrared spectra nagraph, will enable a systematic investigation of of biogenic gases) will be used to guide the explo- system architectures and the diversity of exoplanet ration of exoplanets. atmospheres. An investment of 424 hours with LUVOIR-A would obtain optical spectra of 30 known 221.02 — The role of laboratory experiments and planets for example. For the more massive of these ab initio calculations in exoplanet atmospheric planets we will have previous mass measurements chemistry from Gaia or radial velocity surveys, creating a pow- Julianne I. Moses1 erful data set for testing theories of planet formation, atmospheric evolution, photochemistry, and cloud 1 Space Science Institute (Seabrook, Texas, United States) processes. For newly discovered planets, astrometric Upcoming observations from the James Webb Space observations with HDI, the telescope’s high resolu- Telescope, ARIEL, and other missions and observa- tion imager, or ground-based radial velocity obser- tional campaigns will enable unprecedented char- vations will constrain planet masses. LUVOIR will acterization of exoplanet atmospheric structure and also offer unparalled transit science, particularly at composition, through transit and emission spec- UV wavelengths, enabling studies of photochemistry troscopy acquired at various phases of the planet’s and atmospheric escape. In our poster presentation orbit about its host star. Theoretical models are we will illustrate a few examples of LUVOIR capabil- needed to fully interpret these observations. How- ities with both the A and B architectures to explore ever, such models rely on accurate laboratory and comparative planetary science, illustrating the diver- theoretical inputs that are relevant to the physi- sity of studies possible within a relatively modest ap- cal and chemical conditions of the exoplanets be- plication of observatory time. ing observed. Many of our current inputs are based on Earth atmospheric conditions or other terrestrial 221.04 — Direct Detection of CO in CI Tau b: and solar-system applications that have little resem- Support for Hot Start Formation blance to exoplanet atmospheric conditions. I will This is an additional presentation of abstract 105.04. See review recent advances in laboratory experiments that entry for details. and theoretical ab initio calculations that have im- proved our understanding of exoplanet atmospheric chemistry. I will also describe situations in which 222 — WFIRST Ultra-Deep Fields I insufficiencies in our knowledge of kinetic reaction- rate coefficients, thermodynamic parameters, pho- 222.01 — LSST Deep Drilling Field Program toabsorption cross sections, microphysical and opti- cal properties of ”exotic” hazes, and haze formation Frederica Weiner1 mechanisms are currently limiting our ability to ac- 1 University of Delawae (Newark, Delaware, United States) curately predict exoplanet atmospheric composition. I will present the current plan for LSST Deep Drilling Fields (DDFs) including field selection and expected depth and cadence, as well as the recent proposals

91 for new DDFs and DDF cadences, and describe the structure of galaxies within the epoch of reioniza- process and timeline for finalizing the LSST DDF tion. However, in order to gain a complete picture plans. of the production and escape of ionizing radiation and the nature of the earliest stellar populations, 222.02 — Ultra Deep Field survey with WFIRST we require spectroscopic observations of these dis- tant galaxies in the rest-frame ultraviolet and opti- 1 Anton M. Koekemoer cal. The next generation of ground-based telescopes 1 STScI (Baltimore, Maryland, United States) including the Thirty Meter Telescope, Giant Magel- lan Telescope, and European Extremely Large Tele- WFIRST will enable deep field imaging across much scope will enable sensitive spectroscopic follow up larger areas than those previously obtained with of galaxy photometric candidates uncovered by a Hubble, opening up completely new areas of pa- WFIRST Ultra-Deep survey. Spectroscopic measure- rameter space for extragalactic deep fields including ments of key emission features such as hydrogen cosmology, supernova and galaxy evolution science. Lyman-α and multiple metal lines will enable essen- The instantaneous field of view of the Wide Field In- tial constraints on the nature of massive stars and strument (WFI) is about 0.3 square degrees, which the interstellar medium during the epoch of reioniza- would for example yield an Ultra Deep Field (UDF) tion. I will describe the powerful synergy between a reaching similar depths at visible and near-infrared WFIRST Ultra-Deep Field Survey and ELT spectro- wavelengths to that obtained with Hubble, over an scopic follow-up area about 100-200 times larger, for a comparable in- vestment in time. Moreover, wider fields on scales of 10-20 square degrees could achieve depths com- 223 — Cosmological Probes of parable to large HST surveys at medium depths such as GOODS and CANDELS, and would enable multi- Dark Matter IV epoch supernova science that could be matched in area to LSST Deep Drilling fields or other large sur- 223.01 — What can the dark sector do? vey areas. Finally, achieving HUDF-quality imaging Marc Kamionkowski1 over areas 100x larger than the current Hubble Ul- 1 Johns Hopkins University (Baltimore, Maryland, United States) tra Deep Field area could yield thousands of galax- ies at or beyond z ∼ 8-10, dramatically increasing the Dark matter solves the problems for which it was discovery potential at these earliest epochs of cosmic introduced if it pressureless and has only gravita- time. tional interactions with itself and with ordinary mat- ter. Likewise, dark energy interacts only gravita- 222.03 — Co-ordinating Observations of Deep and tionally but has negative pressure. Still, both parts Ultra-deep Fields Between Observatories of the dark sector could conceivably have proper- ties beyond these minimal requirements. Here I Peter L. Capak1 consider several ways the dark sector might differ 1 Caltech (South Pasadena, California, United States) from the minimal scenario, some of the observational P. Capak will give an overview of the current efforts consequences, and current and possible future con- to co-ordinate observations of Euclid, LSST, Subaru, straints. Specific examples include new long-range and other observatories on potential WFIRST deep interactions for dark matter, baryon–dark-mater in- fields. He will give a list of potential locations forthe teractions, and several dark-energy novelties. deep and ultra-deep WFIRST fields and highlight the pros and cons. 223.02 — Dark Matter and Fusion Samuel McDermott1 222.04 — WFIRST Deep Fields and the ELTs 1 Theoretical Astrophysics, Fermi National Accelerator Laboratory Alice E. Shapley1 (Chicago, Illinois, United States) 1 UCLA (Los Angeles, California, United States) Over the past several years, non-WIMP dark matter An Ultra-Deep Field survey with the Wide Field In- candidates have attracted a surge of interest in the frared Survey Telescope (WFIRST) will uncover un- particle physics community. In this two-part talk, I precedented photometric sample sizes of galaxies will summarize the underlying physics motivation at z>7. These samples will provide important con- for (and observable consequences of) a dark matter straints on the luminosity function and large-scale that is able to form a bound state of fundamental

92 constituents. I will examine the astrophysical im- The generalized dark matter framework provides plications of a dark fermion that can form two-body tools which systematically characterize, in a data- bound states and some ongoing theoretical work to driven way, the cosmic expansion history at range of elucidate the dark sector ingredients necessary to different epochs. Using a principle component anal- lead to ”successful” late-time fusion phenomenol- ysis (PCA) to apply this framework to the entire dark ogy. sector may yield new insight on cosmological axion fields, the Hubble tension, neutrino interactions and 223.03 — How sound are our (ultra-light axion) species, the physical properties of dark matter, and approximations? the nature of dark energy. This talk presents the first steps in developing a generalized dark sector PCA 1 3 2 Daniel Grin ; Jonathan Cookmeyer ; Tristan L. Smith to determine the effective sound speed of the dark 1 Haverford College (Pasadena, California, United States) sector from measurements of the cosmic microwave 2 Swathmore College (Swarthmore, Pennsylvania, United States) background. 3 UC Berkeley (Berkeley, California, United States)

Axions are a promising dark-matter candidate. 224 — Education & History Ultra-light axions (ULAs) are motivated by string scenarios and could mitigate small-scale challenges 224.01 — NASA’s Universe of Learning: to the ΛCDM paradigm. ULAs will be strin- Connecting Learners to the Subject Matter Experts gently tested by future cosmic microwave back- of NASA Astrophysics ground (CMB) experiments and large-scale structure 1 1 surveys. It is challenging to compute cosmological Emma Marcucci ; Brandon L. Lawton ; Janice C. 2 1 2 observables in ULA scenarios, due to the fact that Lee ; Denise A. Smith ; Gordon K. Squires ; Anya A. 3 4 5 the ULA field oscillates on time scales much shorter Biferno ; Kathleen Lestition ; Lynn R. Cominsky 1 than the Hubble time. In past work, an effective fluid Space Telescope Science Institute (Baltimore, Maryland, United approximation (in which axions are modeled as a States) 2 fluid with a structure-suppressing sound speed) is Caltech/IPAC (Pasadena, California, United States) 3 used to make computations feasible and obtain con- NASA JPL (Pasadena, California, United States) 4 straints. Here this approximation is tested against Smithsonian Astrophysical Observatory (Cambridge, Mas- a complete solution of the ULA equations, compar- sachusetts, United States) 5 ing the induced error of CMB observables with the Sonoma State University (Rohnert Park, California, United States) sensitivity of current and future experiments. In the most constrained mass range for a ULA dark matter NASA’s Universe of Learning (NASA’s UoL) is −27 −25 a competitively-awarded program that creates re- component (10 eV ≤ ma ≤ 10 eV), the induced bias on ULA parameters from Planck is less than 1σ. sources and experiences that inspire and enable In the cosmic-variance limit (including temperature learners of all ages and backgrounds explore funda- and polarization data), the potential bias on param- mental questions in science, experience how science eters is 4-10σ at Fisher level; this implies that tests of is done, and discover the universe for themselves. ULAs using data from future efforts like CMB Stage- Using its direct connection to the science and the ex- 4 will require more precise methods. It is also found perts behind the science, NASA’s UoL creates and using the exact and effective fluid calculations that if delivers timely and authentic resources and experi- ULAs compose all the dark matter, the suppression ences for learners. of power relative to standard cold dark matter scales In this presentation, we will provide an overview with wave number as k−8, rather than the often-used of NASA’s UoL and describe our efforts to involve k−16 ‘fuzzy’-dark matter scaling, with possible im- subject matter experts (SMEs) (scientists and engi- plications for small-scale observables. neers) from across the broad range of NASA Astro- physics themes and missions in all of our projects. NASA Astrophysics SMEs are critical to the success 223.04 — Probing the effective sound speed of the of the program because they (1) provide a direct con- dark sector using the CMB nection to the science, (2) ensure accuracy of con- Tristan L. Smith1; Daniel Grin2; David Robinson1; Max tent, and (3) provide learners with a personal con- Aifer2 nection to NASA science. Research and evaluation 1 Swarthmore College (Swarthmore, Pennsylvania, United States) have shown that these direct connections to science 2 Haverford College (Haverford, Pennsylvania, United States) are critical to enhancing learners’ experiences and outcomes. We have identified, with input from the

93 community, a range of ways SMEs can be involved Some 25 resources have already been posted, includ- in providing science expertise to NASA’s UoL prod- ing a list of free on-line videos to go with each chap- ucts and programs. Involvement can include pro- ter (with links), a list of free on-line lab manuals and viding science review, participating in person or re- lab exercises at the level of the book, resources about motely in events, participating in the development of the contributions of women to astronomy and the is- resources, and more. The next step in our work is to sues they face, an introductory manual for the free provide a way to connect SMEs with relevant oppor- Stellarium planetarium software, a primer for first- tunities. We are leveraging existing SME database time instructors, sample syllabi, etc. infrastructure to do just this. During the presenta- tion, we will share the SME database and how par- 224.03 — Astronomy from the Moon: Galaxy First ticipants can register their interest. The database will Light Imaging, Earth Observation provide connections between SMEs and a menu-of- 1 opportunities to engage learners through NASA as- Steve Durst 1 trophysics content and programs. International Lunar Observatory Association (ILOA) (Kamuela, NASA’s UoL is a unique partnership between the Hawaii, United States) Space Telescope Science Institute, Caltech/IPAC, Jet 2019 Astronomy from the Moon continues to expand Propulsion Laboratory, Smithsonian Astrophysical as a promising new frontier for astronomy in the 21st Observatory, and Sonoma State University and is century and as an early ‘light industry’ for the Moon. supported by NASA under cooperative agreement China is pioneering with first robotic telescopes on award number NNX16AC65, as part of the NASA another world with lunar near-side Lunar Ultravi- Science Mission Directorate Science Activation pro- olet Telescope (LUT) aboard the Chang’e-3 station gram. and with lunar far-side Netherlands-China Low Fre- quency Explorer (NCLE) aboard the Chang’e-4 sta- 224.02 — Update on the Non-profit Project to tion – almost a half-century after USA Apollo 16 Produce and Disseminate a Free, Open-source commander John Young obtained astronomical im- Astro 101 Textbook and Resource Hub ages on the lunar surface with a Far-UV spectrograph camera. Indian astrophysicists have expressed inter- Andrew Fraknoi1; David Morrison2; Sidney Wolff3 est in lunar-based astronomy, as have astronomers 1 Fromm Institute, University of San Francisco (San Francisco, in Europe, Japan, Russia, Canada, Korea, as well as California, United States) developing independent enterprises such as the In- 2 NASA Ames (Mountain View, California, United States) ternational Lunar Observatory Association (ILOA) 3 NOAO (Tucson, Arizona, United States) based on Hawai’i. OpenStax (a nonprofit organization based at Rice In observing the Milky Way galactic center, ILOA University) has been working with senior authors chose as the first-light image for its ILO-X and ILO- Andrew Fraknoi, David Morrison, and Sidney Wolff, 1 instruments, from hundreds of Hawaii astronomer and about 70 other members of the astronomical suggestions and considerations, a majestic, inspiring, community, to produce a competitive, free, open- directional, iconic object. The first-ever image of the source Astro 101 textbook. (This is part of a na- Galaxy from the Moon could be as influential and tional program to develop free textbooks in every inspiring as the first image of the Earth ever from the main field in which students take intro classes, and Moon: A look ahead at the human future in the 21st thus help reduce the accelerating cost of a college ed- century out in the Galaxy, like the first look back at ucation.) Approximately 500 instructors and 200,000 the heritage and fragility of spaceship Earth in the students are using the Astronomy textbook this year. 20th. It can be seen and downloaded in a variety of for- Long-duration, high-resolution observation of mats at http://openstax.org/details/astronomy. Earth meteorology, magnetosphere and rotation can A number of ancillary resources have been pro- produce enhanced, unique and highly valuable data duced, including a bank of over 1000 multiple-choice and information across a wide spectrum of interests questions and a wide range of essay type questions. and applications. From solar weather, to navigation The answers are behind a fire-wall for registered accuracy, to commerce, aerospace, defense, as well adopters (but registration is also free, once instruc- as astrophysics and precession information needs for tor status is verified). In addition, an Open Educa- increasingly precise values and expressions for the tion Resource Hub has been assembled for the book, Rotation of the Earth, observation from the Moon, where authors and adopters can share resources. including interferometry and VLBI, provides a new entire world for perspectives on the infinite universe.

94 224.04 — The Explanation for Helium Flashes and The second demo dramatically shows the shape Type Ia Supernovae and origin of phases of the Moon. For this demon- stration, the Sun and Moon must both be visible Kenneth G. Gayley1 1 in a clear sky. Holding a golf or tennis ball with Univ. of Iowa (Iowa City, Iowa, United States) thumb and forefinger in the Moon’s direction magi- cally creates on a “microscopic” scale the same phase It is widely known that the onset of ion fusion in for the ball (crescent, half or gibbous) as for the the presence of highly degenerate electrons results much larger and more distant Moon seen “beside” in nuclear runaway, and that this causes “helium the ball. The Moon and Milky Way demos provide flashes” and type Ia supernovae. This is of interest nice photo/video ops. I acknowledge Ms. Laven- because our own Sun will eventually undergo a he- der’s Tuscaloosa Capitol School 4th grade and the lium flash, and type Ia supernovae provide anim- University of Alabama College of Continuing Stud- portant standard candle for cosmology. These run- ies online Astronomy lab course students for serving away processes are well modeled, but the widely re- as test subjects. See https://www.researchgate. peated conceptual explanation is physically incor- net/profile/Gene_Byrd2 for photos etc. on this and rect, as can be shown from elementary gas physics. other topics. The correct explanation is just as accessible and con- siderably more interesting, as it exposes the remark- able quality of the energy exchange between degen- 224.06 — No Shadow of A Doubt: Dyson, erate and ideal species in thermal contact. In the pro- Eddington and the 1919 Eclipse Expeditions cess, it reveals crucial insights about the contrasting Daniel Kennefick1 thermodynamics of degenerate versus ideal equa- 1 University of Arkansas - Fayetteville (Fayetteville, Arkansas, tions of state. United States)

224.05 — Two Astronomy Demos: Milky Way This is the centenary year of the celebrated eclipse ex- “Stars like Grains of Sugar” and Phases with a peditions of 1919 which confirmed Einstein’s theory Golf Ball, the Sun and the Moon of General Relativity. In recent decades the story of these expeditions has focused on Arthur Stanley Ed- Gene G. Byrd1 1 dington and the question of his alleged bias in favor University of Alabama - Tuscaloosa (Tuscaloosa, Alabama, United of Einstein’s theory. It has been alleged that Edding- States) ton threw out data which did not favor Einstein’s theory. Meticulous examination of the expeditions’ Indoor and outdoor astronomical size/distance papers reveals that this view is mistaken. The rele- demonstrations are well- known, e.g., the huge ratio vant data was taken by the expedition organized by of the Sun’s size versus planets and the separations the Greenwich observatory and it was the director of of the Sun and planets versus their sizes. Here we that observatory, the Astronomer Royal, Frank Wat- discuss two demos showing not sizes but astronom- son Dyson, who was responsible for the decisions ical number and shape. In the first, we have used in question. Studies of the data analysis sheets and grains of sugar to help students appreciate the im- comparison with modern re-analysis of the original mense number of Milky Way Galaxy stars. For an plates vindicate his decision. The story of the two elementary school class, we bought a 5 lb. bag of expeditions,is a remarkable one and this talk will ex- fine-grained sugar. The size of a grain is about 0.1 amine the people, the instruments and the science of mm so a 10x10x10 cm bag would be 1000x1000x1000 the teams and how their work changed science for- grains in length, width and depth.. Multiplying, our ever. bag had about a billion grains, (about the same as the number of stars in a dwarf galaxy). I had the teacher theatrically pour the bag’s grains slowly into 224.07 — The Australian Aborigines Could Easily a container letting the students see and, afterward, Discover the Variability of Betelgeuse, and They feel the ”multitude” of sugar stars in just one bag. Did Discover the Variability . But of course, there are about 100 billion stars in Bradley E. Schaefer1 the disk of our Milky Way Galaxy which is compa- 1 Louisiana State Univ. (Baton Rouge, Louisiana, United States) rable to the grains in a hundred bags of sugar. This is far too many to bring to class! Sand can be used Hamacher (2018) has recently put forth a popular- if available in a conveniently shaped bag. Drawing ized claim that the Australian Aborigines discovered diagrams will help students visualize the estimate. the variability of the red supergiant Betelgeuse, as

95 well as the variability of Aldebaran and Antares. The N. Woods13; Bin Chen14; Dale E. Gary14; Hugh S. basis is that multiple tribal groups around Australia Hudson1; Adam Kowalski13; Alexander Warmuth17; have long-standing lore about the red-star in what- Stephen M. White15; Astrid Veronig18; Nicole Vilmer16 we-now-call Orion that waxes and wanes in bright- 1 NASA GSFC (Washington, District of Columbia, United States) ness, with this all transmitted as a morality tale. 2 Univ of Glassgow (Glassgow, United Kingdom) Other independent traditions are known for indicat- 3 National Astronomical Observatory (Nagoya, Japan) ing the variability of Betelgeuse, Antares, and Alde- 4 Univ of Genoa (Genoa, Italy) baran. This claimed prehistoric discovery of stellar 5 Univ of Colorado (Boulder, Colorado, United States) variability runs up against various (spurious) biases 6 NJIT (Newark, New Jersey, United States) within the historical communities, and there is also a 7 AFRL (Albuquerque, New Mexico, United States) healthy skeptical worry that inexperienced observers 8 Paris Observatory (Paris, France) could not discover the variability. So I have made 9 Leibniz Institute for Astrophysics Potsdam (Germany, Germany) an independent assessment of the claim. I find that 10 University of Graz (Graz, Austria) the claim is good, in that the Aborigines (and any 11 UC Berkeley (Berkeley, California, United States) other group in old times going back many thousands 12 UMN (Minneapolis, Minnesota, United States) of years) could easily have discovered the variabil- 13 SwRI (Boulder, Colorado, United States) ity. The essence is that inexperienced observers can 14 Space Research Centre, Polish Academy of Sciences (Wroclaw, readily note relative brightness changes down to 0.3 Poland) mag in size, while Betelgeuse (and the others) have 15 University of Applied Sciences Northwestern Switzerland excellent comparison stars, so Betelgeuse’ variabil- (Windish, Switzerland) ity from V=0.0 to V=1.3 is easy. Betelgeuse is one 16 NASA MSFC (Huntsville, Alabama, United States) of the most prominent stars in the sky, and so will 17 UMD College Park (College Park, Maryland, United States) be seen often by Aborigines at night in the clear dark 18 Caltech (Pasadena, California, United States) Outback skies. The discovery of variability would have started simply by many people at many times The Focusing Optics X-ray Solar Imager (FOXSI), noting something like Betelgeuse being significantly a SMEX mission concept in Phase A, is the first- brighter than nearby Procyon, while a few months ever solar-dedicated, direct-imaging, hard X-ray tele- earlier it was significantly fainter than Procyon, The scope. FOXSI provides a revolutionary new ap- Aborigines have a long proven track record of turn- proach to viewing explosive magnetic-energy release ing celestial observations into lore that gets passed on the Sun by detecting signatures of accelerated along faithfully down many generations for thou- electrons and hot plasma directly in and near the sands of years. This is all making the case that the energy-release sites of solar eruptive events (e.g., so- Aborigines could discover the variability. The proof lar flares). FOXSI’s primary science objective isto that the Aborigines did discover the variability is sim- understand the mystery of how impulsive energy re- ply that they have documented lore from many tribes lease leads to solar eruptions, the primary drivers of that unambiguously identifies the specific stars as space weather at Earth, and how those eruptions are waxing and waning. energized and evolve. FOXSI addresses three impor- tant science questions: (1) How are particles acceler- ated at the Sun? (2) How do solar plasmas get heated 225 — Solar Physics Division to high temperatures? (3) How does magnetic en- Meeting (SPD), Flares II ergy released on the Sun lead to flares and eruptions? These fundamental physics questions are key to our understanding of phenomena throughout the Uni- 225.01 — The Focusing Optics X-ray Solar Imager verse from planetary magnetospheres to black hole (FOXSI) accretion disks. FOXSI measures the energy distri- Steven Christe1; Albert Y. Shih1; Sam Krucker2; Lind- butions and spatial structure of accelerated electrons say Glesener3; Pascal Saint-Hilaire2; Amir Caspi4; Szy- throughout solar eruptive events for the first time by mon Gburek5; Marek Steslicki5; Joel C. Allred1; Marina directly focusing hard X-rays from the Sun. This nat- Battaglia6; Wayne H. Baumgartner7; James Drake8; urally enables high imaging dynamic range, while Keith Goetz3; Brian Grefenstette9; Iain Hannah10; previous instruments have typically been blinded by Gordon D. Holman1; Andrew Inglis1; Jack Ireland1; bright emission. FOXSI provides 20–100 times more James A. Klimchuk1; Shin-Nosuke Ishikawa11; Ed- sensitivity as well as 20 times faster imaging spec- uard Kontar10; Anna-maria Massone12; Michele troscopy than previously available, probing physi- Piana12; Brian Ramsey7; Richard A. Schwartz1; Thomas cally relevant timescales (<1 second) never before ac-

96 cessible. FOXSI’s launch in July 2022 is aligned with 225.03 — First detection of non-thermal emission the peak of the 11-year solar cycle, enabling FOXSI in a NuSTAR solar microflare

to observe the many large solar eruptions that are ex- 2 1 pected to take place throughout its two-year mission. Lindsay Glesener ; Sam Krucker ; Jessie McBrayer Duncan2; Iain Hannah3; Brian Grefenstette4; Bin Chen5; David M. Smith6; Stephen M. White7; Hugh 225.02 — FOXSI-2 Solar Microflares : S. Hudson1 Multi-Instrument Differential Emission Measure 1 University of California, Berkeley (Berkeley, California, United Analysis States) P. S. Athiray7; Lindsay Glesener1; Juliana Vievering1; 2 University of Minnesota (Minneapolis, Minnesota, United States) Shin-Nosuke Ishikawa2; Andrew Inglis3; Noriyuki 3 University of Glasgow (Glasgow, United Kingdom) Narukage4; Daniel Ryan5; Juan Camilo Buitrago- 4 California Institute of Technology (Pasadena, California, United Casas6; Steven Christe5; Sophie Musset1; Sam Krucker6 States) 5 1 University of Minnesota (Minneapolis, Minnesota, United States) New Jersey Institute of Technology (Newark, New Jersey, United 2 Nagoya University (Tokyo, Japan) States) 6 3 The Catholic University of America (Washington, Washington, University of California, Santa Cruz (Santa Cruz, California, United States) United States) 7 4 National Astronomical observatory of Japan (Tokyo, Japan) Air Force Research Laboratory (Albuquerque, New Mexico, 5 NASA Goddard Space Flight Center (Washington, Washington, United States) United States) We report the detection of emission from a non- 6 University of California, Berkeley (Berkeley, California, United thermal electron distribution in a small solar mi- States) croflare observed by the Nuclear Spectroscopic Tele- 7 NASA Marshall Space Flight Center (Huntsville, Alabama, scope Array (NuSTAR). On 2017 August 21, NuS- United States) TAR observed a solar active region for approxi- mately an hour before the region was eclipsed by The plasma temperature distribution above 5 MK the Moon. The active region emitted several small during microflares is often loosely constrained due microflares of GOES class ∼A and smaller. In this to limited high sensitivity hard X-ray measurements work, we present spectroscopy demonstrating evi- covering the wide range of temperatures observed. dence of electron acceleration in one of these mi- The Focusing Optics X-ray Solar Imager (FOXSI) croflares (GOES class A5.7) and we compare ener- sounding rocket experiment performs direct imag- getic aspects of the accelerated distribution to com- ing and spectroscopy of the Sun in hard X-rays, in monly studied larger flares. The flaring plasma the energy range 4 to 20 keV. FOXSI offers better sen- observed by NuSTAR, with supporting observation sitivity for temperatures above 5 MK by using direct by the Reuven Ramaty High Energy Solar Spectro- focusing grazing incidence X-ray optics, the first of scopic Imager (RHESSI), is well accounted for by a its kind for dedicated solar observations. The sec- thick-target model of accelerated electrons collision- ond FOXSI flight was launched on 2014 December ally thermalizing within the loop, akin to the “coro- 11 and observed microflares, quiescent Sun and qui- nal thick target” behavior occasionally observed in escent active regions. This flight was coordinated larger flares. Future observations of this kind will with the X-ray Telescope (XRT) onboard Hinode and enable understanding of how flare particle acceler- the Atmospheric Imaging Assembly (AIA) onboard ation changes across energy scales, and will aid the SDO which offers unprecedented temperature cov- push toward the observational regime of nanoflares, erage for characterizing the plasma temperature dis- which are a possible source of significant coronal tribution. We present an overview of microflares heating. observed during the FOXSI-2 flight with concurrent brightening observed in Extreme Ultraviolet (EUV) 225.04 — Analyzing Subsecond X-ray Pulsations and soft X-rays, which indicates emission beyond to Probe Particle Acceleration in a Pair of M9.3 10 MK. By combining data from FOXSI-2, XRT, and Class Flares AIA, we determined a well-constrained DEM for the microflares. The coordinated FOXSI-2 observations Trevor Knuth1; Lindsay Glesener1 produce one of the few definitive measurements of 1 School of Physics and Astronomy, University of Minnesota (Min- the distribution and the amount of plasma above 5 neapolis, Minnesota, United States) MK in microflares. Solar flares are large releases of magnetic energy in the solar corona. Studying small timescale (≤ 2s)

97 fluctuations in nonthermal X-ray flux is one possi- and microwave spectral indices and on the modula- ble probe of the particle acceleration mechanisms at tion of the degree of polarization of the radio emis- work. By measuring these timescales and comparing sions. To further constrain the potential QPP mech- them to the predicted acceleration timescales (con- anism, we analyse spatially resolved observations of volved with a time-of-flight timescale) called for by the non-thermal pulsations using both RHESSI and various acceleration mechanisms, a test for their va- Nobeyama RadioHeliograph data to probe the loca- lidity can be made. Additional analysis avenues in- tions of where the QPP emission is occurring. The clude examining the lag between spike peaks across results are suggestive of a trap-plus-precipitation energy bands and the quasi-periodicity of these fluc- model. We will also discuss the QPP modulation in tuations. This work details the analysis of small relation to the observed CME eruption. The current timescale fluctuations in 2 M9.3 solar flares which oc- theories to explain the presence of QPPs in the con- curred on July 30 and August 4, 2011. The method text of this event will be presented, along with a dis- utilized follows the methods described in Kiplinger cussion of how this type of analysis can be further et al. 1983 and Qiu et al. 2012. This study aims utilized to probe the mechanisms for electron accel- to prove the usefulness of Fermi Gamma-ray Burst eration and plasma heating. Monitor (Fermi GBM) data as a means of examin- ing these small timescale fluctuations. Data from 225.06 — Warm-Target Modeling and a Solution to the Reuvan Ramaty High Energy Solar Spectroscopic The Low-energy Cut-off Problem Imager (RHESSI) are used to determine the spectral 1 2 properties of the flare. As Fermi does not use the A. Gordon Emslie ; Eduard Kontar ; Natasha L S 2 rotation-based imaging system that RHESSI does, Jeffrey 1 time profiles do not require intensive demodulation. Western Kentucky University (Bowling Green, Kentucky, United This study will assist in having Fermi GBM data play States) 2 a greater role in high energy solar flare research mov- Physics & Astronomy, University of Glasgow (Glasgow, United ing forward. Kingdom) Solar flare hard X-ray (HXR) spectroscopy serves asa 225.05 — Temporal, Spectral and Spatial Analysis key diagnostic of the accelerated electron spectrum. of Flaring Quasi-Periodic Pulsations However, the standard approach using the colli- Laura A. Hayes1; Peter Gallagher2; Steven Christe1; sional cold thick-target model poorly constrains the Brian R. Dennis1 lower-energy part of the accelerated electron spec- 1 NASA Goddard Space Flight Center (Washington DC, District of trum, hence the overall energetics of the accelerated Columbia, United States) electrons and consequently the flare energetics are 2 Astronomy & Astrophysics Section, Dublin Institute of Advanced typically constrained only to within one or two or- Studies (Dublin, Ireland) ders of magnitude. I will discuss the development and application of a physically self-consistent, warm- One of the key observational features in flaring emis- target approach that involves the use of both HXR sion associated with accelerated electrons is the pres- spectroscopy and imaging data. The approach al- ence of pronounced modulations and oscillatory sig- lows an accurate determination of the electron dis- natures known as quasi-periodic pulsations (QPPs). tribution low-energy cutoff, and hence the electron To date, the underpinning mechanisms resulting in acceleration rate and the contribution of accelerated the emission modulation remains unknown, and electrons to the total energy released, by constrain- detailed multi-wavelength investigations of flaring ing the coronal plasma parameters. Using a solar QPP events are required to identify the modulation flare observed in X-rays by RHESSI, we demonstrate process. Here we will present a detailed temporal, that using the standard cold-target methodology, the spectral and spatially-resolved investigation of the low-energy cutoff (hence the energy content in elec- X1.2 solar flare from May 15 2013 that demonstrate trons) is essentially undetermined. However, the large modulations in its emission. During the im- warm-target methodology can determine the low- pulsive phase, pronounced QPPs with a period of energy electron cutoff with ∼7% uncertainty at the 50s are observed across multiple wavebands includ- 3σ level, hence it permits an accurate quantitative ing hard and soft X-rays, microwave, UV, EUV - es- study of the importance of accelerated electrons in sentially across the whole flaring region. We ex- solar flare energetics. amine the modulation amplitudes of the different emissions, and in particular focus on the hard X-ray

98 226 — Solar Physics Division lead to counter-propagating waves that should in- duce turbulence and subsequent dissipative heating. Meeting (SPD), DKIST I Using methods like local correlation tracking (LCT) and feature tracking to infer flows in rapid-cadence, 226.01 — Status of the Daniel K. Inouye Solar high-resolution DKIST observations of magnetized Telescope regions of the lower solar atmosphere should enable testing these, and other, coronal heating models. Thomas R. Rimmele1 1 National Solar Observatory (Boulder, Colorado, United States) 226.03 — Filament Magnetic Fields at the DST and The construction of the 4m Daniel K. Inouye Solar DKIST Telescope (DKIST) on Haleakala, Maui is in its final 1 2 3 phase. The construction of the facility is 90% com- Shuo Wang ; Jack Jenkins ; Valentin Pillet ; Christian 3 2 4 plete. Operations are scheduled to begin in 2020. Beck ; David Long ; Debi Prasad Choudhary ; James 1 DKIST was designed to meet the needs of critical McAteer 1 high resolution and high sensitivity spectral and po- Department of Astronomy, New Mexico State University (Las larimetric observations of the sun. The design allows Cruces, New Mexico, United States) 2 DKIST to operate as a coronagraph at infrared wave- Mullard Space Science Laboratory, University College London lengths where the sky background is low and bright (London, United Kingdom) 3 coronal emission lines are available. Taking advan- National Solar Observatory (Boulder, Colorado, United States) 4 tage of its large aperture and infrared polarimeters Department of Physics & Astronomy, California State University DKIST will be capable to routinely measure the cur- (Northridge, California, United States) rently illusive coronal magnetic fields. The state-of- Observations from the 0.8-m Dunn Solar Telescope the-art adaptive optics system provides diffraction (DST) are qualitatively similar to data that will be limited imaging and the ability to resolve features produced by the 4-m Daniel K. Inouye Solar Tele- approximately 20 km on the Sun. Five first light in- scope (DKIST), albeit at a lower spatial resolution struments will be available at the start of operations. and polarimetric sensitivity. We present HAZEL in- The data from these instruments will be distributed versions of spectropolarimetric observations of a qui- to the community via the NSO/DKIST data center escent filament acquired with the Facility Infrared located in Boulder. We will discuss the project sta- Spectropolarimeter at the DST. This study includes tus. three observations of the He I triplet at 10830 Å on May 29 and 30, 2017. The filament was stable on 226.02 — Photospheric Flows & DKIST: Resolving May 29, and was observed in the process of rising Both Smaller Scales And Open Questions at speeds of 20-30 km/s during the two spatial maps Brian Welsch1 taken on May 30. Vector magnetic fields along the fil- 1 Natural & Applied Sciences, University of Wisconsin - Green Bay ament were obtained that show an inverse configura- (Green Bay, Wisconsin, United States) tion indicative of a flux rope topology, including co- aligned threads. To take advantage of the better spa- The technical aim of DKIST is to resolve dynam- tial and temporal resolution of the DKIST, future col- ics on spatial scales not yet observed — an achieve- laborations of the DKIST and the DST to study solar ment that also promises to resolve many impor- filaments are discussed. We propose to further study tant science questions. For instance, the characteris- the evolution of solar filaments that erupt and lead tics of photospheric velocity fields on currently un- to Coronal Mass Ejections using interspaced obser- resolved scales — such as the strength of vortic- vations from the DKIST and DST spectropolarime- ity present, and the lifetimes of flow patterns — ters. While the DST observations will give informa- have substantial implications for theories chromo- tion about the global evolution of physical proper- spheric and coronal heating. Parker long ago hy- ties leading to the destabilization, the DKIST obser- pothesized that the braiding of flux tubes by pho- vations will provide the information about the phys- tospheric flows might play a role in the generation ical conditions in the small-scale structures that sup- of current sheets above the photosphere, whose dis- port the filament material. sipation should lead to atmospheric heating. More recently, van Ballegooijen and collaborators have 226.04 — Labeling Known Unknowns in the proposed that photospheric flows evolving on time Chromosphere Through Forward Modeling scales shorter than the round-trip, photosphere-to- transition-region travel time for Alfven waves could Donald James Schmit1

99 1 Physics Dept, Catholic University (Washington, District of with the maximum-likelyhood solution for the pa- Columbia, United States) rameters of the underlying atmosphere. Inversions are extremely numerically demanding, because they Spectroscopy provides one of the basic diagnostic fully take into account all the physical processes in- means of deriving the thermodynamic properties of volved in the spectral line formation. This is es- astrophysical plasmas. Chromospheric spectral lines pecially pronounced in the case of spectral lines of cool stars like the Sun are an unique diagnostic formed in the solar chromosphere. With the ad- challenge: they are optically thick and formed under vent of next generation telescopes, such as DKIST, non-LTE conditions. In this work, we study chro- standard, minimization-based, inversions will sim- mospheric line formation using a forward model- ply be too slow. In this contribution we propose a ing approach. We use the Bifrost stellar atmosphere way to accelerate the inversions by means of convo- simulation to generate 340000 profiles pairs in two lutional neural networks. We invert a small sub-set related transitions: Ca II 8542A and Mg II 2803A. of the data using standard inversion approach and This synthetic dataset is a powerful tool because we then train a convolutional neural network to gener- know both the properties of the emitting plasma (the alize the results to the full data set. We analyze this unknown in remote sensing) and the emergent pro- method on different synthetic and observed data sets file (the observable). We use this dataset to address and compare the results with the results obtained by two questions: 1) Which kinds of profiles occur most applying standard inversion methods. We find that, commonly in the simulation? 2) How much infor- given an extensive enough data set, convolutional mation overlap exists between the 8542A and 2803A neural networks provide results that are very close profiles? Our research into the first question sug- to the ones obtained by standard inversion methods, gests that a substantial degree of degeneracy exists in a fraction of time. for chromospheric profiles: a wide range of atmo- spheres can generate similar profiles in a 2D or3D 226.06 — Magnetic reconnection in the low hydrodynamic system. If a single profile does not atmosphere: Ellerman bombs and UV bursts provide a satisfactorily narrow distribution of atmo- spheric properties then a logical progression is to Peter R. Young1 use more than one line. We use Bayes theorem to 1 NASA Goddard Space Flight Center (Greenbelt, Maryland, address to what degree the more broadly-affected United States) 2803A spectral profile can predict the spectral profile of the 8542A line. While the wings of 8542A are pre- Ellerman bombs (EBs) were first discovered over a dicted with high efficacy from a sample Mg II profile, hundred years ago and are widely interpreted as we find the Doppler shifts in the line core and line magnetic reconnection events occurring deep in the core emission are not predictable by our direct use atmosphere. UV bursts have been actively studied of Bayes theorem. This implies that multiple chro- since the launch of IRIS in 2013 and show many sim- mospheric lines, even if they ”form” in similar re- ilarities to EBs, but significantly give a strong signa- gions, do contain non-redundant information. Our ture in the Si IV emission lines that indicate hotter results suggest that multi-instrument datasets and temperatures. The interpretation is again magnetic the application of machine learning techniques hold reconnection, but in a higher layer of the atmosphere promise to advance our understanding of the chro- or with a different magnetic geometry. mosphere. The expected small spatial scales of magnetic re- connection, and the tantalizing hints from recent 226.05 — Mimicking spectropolarimetric high resolution ground observations suggest that inversion using convolutional neural networks EBs and UV bursts will be an ideal demonstration of DKIST’s capabilities. This talk summarizes recent Ivan Milic1; Ricardo Gafeira2 results on EBs and UV bursts and identifies key ob- 1 CU Boulder / LASP (Boulder, Colorado, United States) servational capabilities of DKIST. 2 Instituto Astrofisica de Andalucia (Granada, Spain)

State of the art approach for the interpretation of spectropolarimetric observations of the solar atmo- sphere are the so called spectropolarimetric inver- sions. These methods fit a model atmosphere to the observed polarized spectrum and provide us

100 227 — Plenary Lecture: TBD, 1 Yale University (New Haven, Connecticut, United States) 2 Elisabeth Mills (Brandeis Modulos AG (Zurich, Switzerland) University) We examine morphology-separated colour-mass di- agrams to study the quenching of star formation in ∼100,000 SDSS (z∼0) & ∼20,000 CANDELS (z∼1) 227.01 — Journey to the Center of the Galaxy: galaxies. To classify galaxies morphologically, we Following the Gas to Understand the Past and developed Galaxy Morphology Network (GaMor- Future Activity of Galaxy Nuclei Net), a convolutional neural network that can clas- Elisabeth A. Mills1 sify galaxies according to their bulge-to-total ratio. 1 Brandeis University (Waltham, Massachusetts, United States) GaMorNet does not need a large training set of real data and can be applied across multiple data-sets to Centers of galaxies are some of the most extreme ob- do morphological classification. GaMorNet’s source jects in our universe: hosting starbursts and active code as well as the trained models are made public supermassive black holes that can launch jets and as part of this work. We first trained GaMorNet on winds far outside the compact galaxy nucleus. The simulations of galaxies with a bulge and a disk com- effects of the unique interactions between stars, gas, ponent and then transfer learned using ∼25% of each and black holes that occur here don’t just stay con- data set to achieve net accuracies > 91%. The mis- fined to these small regions: they have an outsized classified sample of galaxies is dominated by small influence on the overall evolution of galaxies asa galaxies with low S/N ratios. We find that both sam- whole. At just 8.1 kpc away, the center of the Milky ples of bulge- and disk-dominated galaxies have dis- way is unparalleled in its proximity, making it the tinct colour mass diagrams in agreement with pre- best laboratory for detailed studies of the processes vious studies. For both samples, a) disk-dominated that govern and define galaxy nuclei. However, the galaxies peak in the blue cloud with a slowly de- Galactic center also presents a big challenge for these clining tail that extends through the green valley studies: it is a relatively quiet environment. Few to the red sequence and is consistent with slow ex- stars are forming in this region, and the black hole haustion of gas with no rapid quenching; b) bulge- is not active. Clearly, it hasn’t always been this way: dominated galaxies clearly show a dip in the green from the Fermi Bubbles to hundred-year old echoes valley while peaking in the red sequence suggesting of X-ray bursts there are many relics of an active past rapid quenching and fast evolution across the green in the center of our own Milky Way. We also know valley. our Galaxy center likely won’t stay quiet for long: it contains a sizable reservoir of molecular gas that is 228.02 — (withdrawn) the fuel for future star formation and black hole ac- cretion. In this talk I will present the results of re- This abstract was withdrawn. search following the gas and its properties from kilo- parsec to sub-parsec scales to understand why the 228.03 — New Content and Functionality in NED: Galactic center is so quiet right now and what the fu- Summer 2019 Update ture holds. Finally, I will discuss ongoing work to double and triple the sample size of galaxy nuclei Joseph M. Mazzarella1; Xiuqin Wu1; Barry F. Madore1; with sub-parsec scale gas measurements, and what George Helou1; Marion Schmitz1; David O. Cook1; Xi this means for putting the Galactic center in context Chen1; Rick Ebert1; Jeffery D. Jacobson1; Scott Terek1; with its more active neighbors. Tak M. Lo1; Hiu Pan Chan1; Olga Pevunova1; Cren Frayer1 1 Caltech (Pasadena, California, United States) 228 — iPoster Plus VIII: Supernovae, AGN & Galaxies The NASA/IPAC Extragalactic Database (NED) is undergoing a major expansion in data content and functionality improvements. A fusion of attributes 228.01 — Galaxy Morphology Network for prior objects in the system with fundamental (GaMorNet): A Convolutional Neural Network to measurements from NASA’s GALEX, 2MASS and study morphology and quenching in ∼100,000 ALLWISE sky surveys, as well as source catalogs SDSS & ∼20,000 CANDELS galaxies from the Spitzer, Hubble and Chandra Space Tele- Aritra Ghosh1; C. Megan Urry1; Zhengdong Wang1; scopes and data joined from over 114,000 journal ar- Kevin Schawinski2; Dennis Turp2; Meredith Powell1 ticles, is vastly increasing the opportunities for mul-

101 tiwavelength research and discoveries. We will re- Our one square degree imager and most produc- view highlights of recent additions to the database, tive instrument, MegaCam, can deliver exquise im- demonstrate capabilities of the new user interface, age quality in the u’ band with unprecedented sen- and summarize current plans for the future that are sitivity. It is also equiped with an ultrawide gri filter being refined with further input from the commu- that can be used for asteroid detection. The camera nity to prepare for the 2020s. NED is operated by also offers a suite of state of the art filters that records the California Institute of Technology, under contract high quality images with broad band g’, r’, i’ and z’ with the National Aeronautics and Space Adminis- filters and narrow band Hα, Hα-off, [O III], [O III]-off tration. and CaHK filters. All together, the science that can be done with the camera is quite broad, ranging from 228.04 — AGN Feedback from Precessing Jets on the study of low metallicity stars in the Milky Way the Turbulent Intracluster Medium to the study of dark matter and dark energy at high redshift using gravitational lensing and supernovae. 1 1 Yinghe Lu ; Paul M. Ricker SITELLE, a Fourier Transform Imaging Spectrograph 1 University of Illinois, Urbana-Champaign (Urbana, Illinois, and ESPaDOnS, an R70k spectropolarimeter com- United States) plete our suite of optical instrumentation. SITELLE can observe up to 4 million spectra simultaneously To study feedback from active galactic nuclei (AGNs) ′ in hydrodynamical simulations of isolated galaxy over a 11 FOV at a resolution ranging from 2 to 9000. cluster environments, we have developed a new sink This very powerful and novel instrument is most use- particle model for supermassive black hole (SMBH) ful for the study of extended emission line objects in accretion and jet launching. Using the new model, the Galaxy or at higher redshift. On the other hand, we have run simulations of the cores of clusters with ESPaDOnS can derive magnetic fields, metal content and even find exoplanets around local stars. Inthe the hydrodynamic code FLASH. We compare our ′ jets to numerical simulations of accretion disks and NIR, CFHT offers two instruments, WIRCam, a20 jets in regions close to SMBHs and investigate the FOV camera and SPIRou, a newly commissioned NIR convergence of our model. We also study the interac- R65k resolution high precision velocimeter and spec- tion of precessing AGN jets, driven turbulence, and tropolarimeter. Both instrument observe from Y to K radiative cooling, aiming to determine the amount of and have the capability to find and characterise exo- turbulence produced by jet feedback and whether it planets. can help regulate accretion. The results are impor- tant for addressing the question of how AGN jets de- 230 — iPoster Plus XII: Cosmology posit energy into the intracluster medium in a dis- tributed manner. 230.01 — Estimating Astrometric Anomalies and Redshift with Evolutionary Physical Constants 229 — iPoster Plus X: Rajendra P. Gupta1 Instrumentation Space, Ground 1 Macronix Research Corporation (Ottawa, Ontario, Canada) and Computation We have developed a cosmological model by allow- ing the speed of light c, gravitational constant G and 229.01 — Overview of the science capabilities of cosmological constant Λ in the Einstein filed equa- the Canada-France-Hawaii Telescope. tion to vary in time, and solved them for Robertson- Walker metric. Assuming the universe is flat and Daniel Devost1 matter dominant at present, we obtain a simple 1 Canada-France-Hawaii Telescope (Kamuela, Hawaii, United model that can fit the supernovae 1a data with a sin- States) gle parameter almost as well as the standard ΛCDM I will give a quick overview of the science capabilities model with two parameters, and has the predictive of the suite of instruments available at the Canada- capability superior to the latter. The model, together France-Hawaii Telescope. The telescope capabalities with the null results for the variation of G from the go from UV wide field imaging to NIR high reso- analysis of lunar laser ranging data determines that lution spectropolarimetry and velocimetry. Twenty at the current time G and c both increase as dG/dt nights are available on five instruments for obser- = 5.4GH0 and dc/dt = 1.8cH0 with H0 as the Hub- vations in Queue Scheduled Observing mode every ble constant, and Λ decreases as dΛ/dt = -1.2ΛH0. semester.

102 This variation of G and c is all what is needed to ac- 301 — Instrumentation: Space count for the Pioneer anomaly, the anomalous secu- lar increase of the Moon eccentricity, and the anoma- Missions Poster Session lous secular increase of the . We also show that the Planck’s constant h increases as 301.01 — A Modified Kirkpatrick-Baez Design for a Practical Astronomical X-ray Telescope dh/dt = 1.8hH0 and the ratio D of any Hubble unit to the corresponding Planck units increases as dD/dt Dana Longcope1; Loren W. Acton1; Charles Kankelborg1 = 1.5DH . We have shown that it is essential to con- 0 1 Montana State Univ. (Bozeman, Montana, United States) sider the variation of all the physical constants that may be involved directly or indirectly in a measure- Kirkpatrick-Baez (K-B) optics offer a means of imag- ment rather than only the one whose variation is be- ing soft x-rays with modest resolution and a multi- ing considered. With this approach we will present arc-minute field of view at a cost far below the con- the current status of our work on how universe may ventional Wolter design. Such a low-cost system have evolved from zero rather than from infinity (i.e. could be useful for dedicated, long time-line obser- singularity) and on the formation of large structures vation of astronomical x-ray sources from orbit. A – galaxies, clusters, and superclusters. K-B telescope consists of crossed arrays of parabolic mirrors at grazing incidence. The classic K-B design 300 — Plenary Lecture: Transiting is subject to significant aberration, arising from in- terplay between the focusing of the fore and aft mir- Exoplanets: Past, Present, & ror arrays. We demonstrate here a modified K-B de- Future, Joshua Winn (Princeton sign with aberrations reduced by an order of mag- nitude. We show, furthermore, that it is possible to University) construct such a system by constraining flat “slats” of commercially-available glass in precision machined 300.01 — Transiting Exoplanets: Past, Present, & grooves. The slats deform into shapes which ad- Future equately approximate the optimal figures, thereby yielding focusing better than the best version of the 1 Joshua N. Winn classic K-B design. The result is a new approach that 1 Princeton University (Cambridge, Massachusetts, United States) greatly simplifies the task of achieving both useful resolution and high effective area for x-ray astron- NASA’s Kepler and K2 missions made major ad- omy applications. vances in exoplanetary science, by detecting thou- sands of transiting planets with a level of photomet- ric precision only possible with space-based observa- 301.02 — Characterization of Carbon Nanotubes tions. These missions revealed strange and unantic- for use as Field Emission Sources on MiniEPMA ipated planetary systems, while also finding planets Collin Flynn1,2 that resemble the Earth in key respects. However, 1 Physics, Coe College (Racine, Wisconsin, United States) the Kepler telescope only monitored 5% of the celes- 2 NASA Goddard Space Flight Center (Greenbelt, Maryland, tial sphere, leaving most of the nearest and bright- United States) est stars unexplored. The Transiting Exoplanet Sur- vey Satellite (TESS) takes the next logical step by per- Aerospace technology has constantly moved to- forming a nearly all-sky survey. The survey began in wards efficiency and miniaturization. Efficiency July 2018. At this point, more than 500 planet candi- is particularly important for deep space missions, dates have been identified, and are being confirmed where is lacking. The Mini Electron Probe through a world-wide effort with ground-based tele- Micro Analyzer (MiniEPMA) is a highly efficient scopes. More generally, TESS explores the bright flight concept capable of spatially mapping theel- and variable sky, including comets and asteroids, emental composition of a mineral target on an air- stellar flares and pulsations, novae and supernovae. less body (e.g. a comet, asteroid, or moon). The MiniEPMA’s efficiency is largely due to its useof carbon nanotubes (CNTs), which are extremely effi- cient at generating electrons compared to other mate- rials commonly used as field emission sources, such as lanthanum hexaboride (LaB6) and tungsten fila- ments. The instrument uses a 10 by 10 addressable

103 array of CNT pillars approximately 100 µm in diam- NASA for study for consideration in the upcoming eter. However, not all CNT arrays are alike. We Astrophysics Decadal Review expected in 2020. In have found very different field emission capabilities order to fit inside the NASA cost guidelines, aOST among CNT arrays that underwent different growth Baseline Mission Concept has been developed that conditions, such as catalyst type, catalyst thickness, consists of a 5.9m diameter telescope that is cooled and the time and gas concentration used during the to 4.5K and a mission that will be optimized for ef- growth. The effects of the growth conditions on field ficient mid and far-infrared astronomical observa- emission were studied with a focus on performance tions. An initial suite of three focal plane instruments and longevity, as well as uniformity within the array. was chosen for the Baseline version of this observa- tory. The Mid-Infrared Transit Spectrometer (MISC) 301.03 — HaloSat: The Case of the Missing instrument will observe at the shortest wavelengths Baryons of any of these instruments, ranging from 2.8 to 20 microns and is optimized for measurements of bio- 1 Rebecca Ringuette signatures in the atmospheres of transiting exoplan- 1 Physics and Astronomy, University of Iowa (Iowa City, Iowa, ets. This wavelength range allows measurements of United States) the surface temperatures of the exoplanets as well as Baryonic matter provides the substance of all the detections of the bio-signature molecules O3, CH4, matter in the universe that is familiar, including peo- H2O, CO2, and N2O at Earth-levels, should they ex- ple, planets, and . However, current calcula- ist in an exoplanet atmosphere. A dichroic beam- tions indicate about one-third of the baryons in the splitter picks off 2.0-2.8 micron light from the host universe to be missing. One possible place baryons star and sends it to a small detector array that is used can ‘hide’ from detectors is in the hot halos surround- to provide fine pointing correction signals to atip- ing galaxies. As the closest galaxy available, the tilt mirror in the telescope optics. The MISC instru- Milky Way Galaxy provides the best halo for study of ment has a densified pupil spectrometer design with diffuse x-ray emission. Currently orbiting, HaloSat is R∼50-300 and is capable of exoplanet transit and the first CubeSat funded by NASA to accomplish an emission spectroscopy with spectro-photometric sta- astrophysical mission: determine whether there is a bility as low as 5 ppm. This allows at least 3.6-σ de- significant presence of baryonic matter in galactic ha- tections of all the lines of interest in 85 transits of a los in light of the missing baryon problem. At a tem- K=9.8 magnitude M-star. This presentation covers perature of about 106 K, the hot halo of the Galaxy the design and expected performance of this instru- provides strong emission lines from O-VII and O- ment when observing exoplanet transits of M stars. VIII at 561 eV and 653 eV. We adapted off-the-shelf low energy x-ray instrumentation to the low-cost for- 301.05 — Updates on the Performance and mat of a CubeSat with additional modifications to Calibration of HST/STIS fulfill our mission goals. Recently, HaloSat accom- 1 1 1 plished full design sensitivity for the measurement S. Tony Sohn ; Doug Branton ; Joleen K. Carlberg ; John H. Debes1; Susana E. Deustua1; Sean A. of the oxygen lines in the halo and continues to col- 1 1 1 lect data. The in-flight calibration of the instrument Lockwood ; Matthew Maclay ; TalaWanda R. Monroe ; Charles R. Proffitt1; Allyssa Riley1; Daniel Welty1 will also be discussed, along with background cuts 1 and subtraction methods. STScI (Baltimore, Maryland, United States) The Space Telescope Imaging Spectroscope (STIS) 301.04 — MISC — An Exoplanet Transit has been on board the Hubble Space Telescope (HST) Spectrometer for the Origins Space Telescope for over 20 years and continues to produce high Thomas L. Roellig1; Itsuki Sakon2; Kimberly Ennico1; quality data. The instrument’s diverse capabilities Taro Matsuo3; Tomoyasu Yamamuro4; Yuji Ikeda5 include spatially resolved spectroscopy in the UV 1 NASA Ames Research Center (Moffett Field, California, United and optical, high spectral resolution echelle spec- States) troscopy in the UV, and solar-blind imaging in the 2 University of Tokyo (Tokyo, Japan) UV. STIS also supports unique visible-light corona- 3 Osaka University (Osaka, Japan) graphic modes that keep the instrument at the fore- 4 Optcraft Corp (Tokyo, Japan) front of exoplanet and debris-disk research. The in- 5 Photocoding (Tokyo, Japan) strument’s characteristics evolve over time, and the STIS branch at the Space Telescope Science Insti- The Origins Space Telescope (OST) is one of four po- tute (STScI) monitor its performance and continually tential flagship missions that have been funded by

104 work to optimize its data products. In this contribu- and a polarized standard GSC 08169-01120 (V∼13.4 tion, we present updates on: (1) the performance of mag), we re-estimate the coefficients required for the STIS CCD and FUV & NUV MAMA detectors; (2) transforming ACS/WFC images using the POLV0, the calibrated science products delivered by CalSTIS; POLV60, and POLV120 filters into Stokes I, Q, and U (3) the STIS Data Handbook; (4) the calibration of the images, along with extracting the polarization frac- spectral sensitivity, including a program to derive a tion and angle. We further discuss the science use- new sensitivity curve for E140M; and (5) other recent cases for the ACS polarization filters in the era of joint user-relevant issues. HST and James Webb Space Telescope observations.

301.06 — Seventeen Years of the Hubble Space 301.08 — Trace and Wavelength Calibrations of Telescope’s Advanced Camera for Surveys: the HST/ACS G800L Grism Calibration Update Nimish P. Hathi1; Norbert Pirzkal1; Norman A. Norman A. Grogin1 Grogin1; Marco Chiaberge1 1 Space Telescope Science Institute (Baltimore, Maryland, United 1 STScI (Baltimore, Maryland, United States) States) The HST/ACS G800L grism, an optical slitless spec- The Advanced Camera for Surveys (ACS) has been troscopy mode on ACS, has been very stable since a workhorse Hubble Space Telescope (HST) imager its inception in 2002, but no major effort to improve for over seventeen years, subsequent to its Servic- its trace and wavelength calibrations has been at- ing Mission 3B installation in 2002. The once defunct tempted since 2005. The accurate calibration of the ACS Wide Field Channel (WFC) has now been oper- spectral trace and the dispersion solution are crucial ating over twice as long (>10yrs) since its Servicing to locate the spectrum in the grism image as well as to Mission 4 (SM4) repair than it had originally oper- precisely identify spectral features in a spectrum. We ated prior to its 2007 failure. Despite the accumu- obtained new observations of an emission line Wolf- lating radiation damage to the WFC CCDs during Rayet star (WR96) in the HST Cycle 25 (PID: 15401) to their long stay in low Earth orbit, ACS continues to undertake a thorough analysis of verifying and im- be heavily exploited by the HST community as both proving the ACS grism calibrations. To account for a prime and a parallel detector. the field dependence, we observed WR96 at 3 differ- We present results from long-term monitoring of ent observing positions over the ACS field of view, WFC dark current and readout noise, results from but that is inadequate coverage to properly sample new studies of detector performance for both WFC the entire ACS field of view. To account for that, and the ACS Solar Blind Channel (SBC), and updated we are uniformly reprocessing all the archival ACS ACS software tools for the user community. High- grism data of WR96. By combining all of the avail- lights include: 1) a WFC readout simulator tool that able data we can now derive a more finely sampled accurately reproduces the effects of degraded WFC field dependence of the grism dispersion solutions. charge transfer effeciency (CTE); 2) color-dependent These data, combined with a new approach to solv- aperture corrections for SBC point-source photome- ing for the polynomial coeffcients of the field depen- try; and 3) a refined WFC geometric distortion solu- dence of both the trace and wavelength calibrations, tion, exploiting precise astrometry of the ACS astro- allow us to improve the accuracy of the grism cali- metric calibration field (globular cluster 47 Tucanae) bration. We will present the latest results from this provided by GAIA DR2. analysis.

301.07 — Calibration of the HST ACS/WFC Linear 301.09 — Assessing the Accuracy of Relative Polarization Filters Photometry on Saturated Sources with ACS/WFC Tyler D. Desjardins1 Melanie Kae Batara Olaes1 1 Space Telescope Science Institute (Baltimore, Maryland, United 1 Space Telescope Science Institute (Baltimore, Maryland, United States) States)

We present the calibration of the Hubble Space Upon full-well saturation, the pixels on the Telescope (HST) linear polarization filters for the ACS/WFC CCDs will bleed excess charge onto Advanced Camera for Surveys Wide Field Chan- adjacent pixels along their column. For these sat- nel (ACS/WFC). Using observations of the bright urated sources, aperture photometry may report (V∼11.7 mag), unpolarized white dwarf G191-B2B a lower flux than expected. However, this affect

105 can be mitigated by defining an extraction aperture of their atmospheres, and obtain information about which encompasses all of the pixels which contain their surfaces. LUVOIR can also observing poten- the full-well bleed. Here we present a functional tially habitable exoplanets transiting nearby M dwarf assessment of relative photometry of saturated stars. Such observations will allow us to evaluate sources from observations of globular cluster 47 these worlds’ habitability and search for the pres- Tuc. Given a successful identification of pixels ence of remotely detectable signs of life known as which contain the lost flux, we demonstrate an “biosignatures.” We will discuss the strategies for alternate method of aperture photometry where Exo-Earth detection and characterization, including >90% accurate photometry of saturated stars can specific observational requirements for astrobiologi- still be obtained out to 2 magnitudes brighter than cal assessments of exoplanetary environments with the standard method. LUVOIR. The survey of the atmospheric composi- tion of dozens of potentially habitable worlds would 301.10 — Focus-Diverse, Empirical PSF models for bring about a revolution in our understanding of the Hubble Space Telescope ACS/WFC planetary formation and evolution, and may usher in a new era of comparative astrobiology. Andrea Bellini1; Jay Anderson1; Norman A. Grogin1; Nathan Miles1 1 301.12 — The Capabilities of LUVOIR for Studies STScI (Baltimore, Maryland, United States) of Exoplanet Diversity Accurate Point-Spread Function (PSF) models are This is an additional presentation of abstract 221.03. See critical in a large variety of science investigations, that entry for details. from stellar photometry and astrometry to galaxy deconvolution. Focus variations, primarily due to 301.13 — Overview of the LUVOIR Space uneven Sun and Earth heating of the Hubble Space Observatory Concepts Telescope but also to outgassing of the metering truss, have a significant impact on the shape of the Aki Roberge1; Debra Fischer2; Bradley M. Peterson3 ACS/WFC PSFs. These variations have been largely 1 NASA GSFC (Greenbelt, Maryland, United States) overlooked since the installment of the ACS in 2002. 2 Yale University (New Haven, Connecticut, United States) Now that thousands of images have been collected 3 Ohio State University (Columbus, Ohio, United States) by the ACS/WFC over the past 17 years in many fil- ters, we can analyze them in a self-consistent way The Large UV/Optical/IR Surveyor (LUVOIR) is a and derive focus-diverse, empirical PSF models that concept for a highly capable, multi-wavelength space we show to be superior to any prior library PSF observatory with ambitious science goals. This mis- models. These new PSF models will be soon made sion would enable great leaps forward in a broad publicly available to the astronomical community range of science, from the epoch of reionization, through easy-to-use Python tools within the STScI through galaxy formation and evolution, star and astropy/photutils package. planet formation, to solar system remote sensing. LUVOIR also has the major goal of characterizing a wide range of exoplanets, including those that might 301.11 — The Search for Biosignatures and be habitable – or even inhabited. But perhaps LU- Exo-Earths with the LUVOIR Mission Concept VOIR’s most important scientific capability is its abil- Giada Arney1 ity to address the science questions of the 2040s and 1 NASA Goddard Space Flight Center (Greenbelt, Maryland, beyond that scientists have not yet thought to ask. United States) Here we provide a high-level overview of the cur- rent LUVOIR observatory architectures. Two vari- The Large Ultra Violet-Optical-Infrared (LUVOIR) ants are being designed in preparation for the As- Surveyor is one of four mission concepts being stud- tro2020 Decadal Survey. LUVOIR-A features a 15- ied by NASA in preparation for the 2020 Astro- m diameter on-axis primary mirror and LUVOIR-B physics Decadal Survey. LUVOIR is a general- has an 8-m off-axis primary mirror. Four candidate purpose space-based observatory with a large aper- instruments are being studied: 1) A NUV to NIR ture (8-15 m) and a total bandpass spanning from high-performance coronagraph (ECLIPS), 2) a wide- the far-UV to the near-infrared. One of LUVOIR’s field NUV to NIR imaging camera (HDI), 3) aFUVto main science objectives is to directly image temperate optical multi-resolution, multi-object spectrograph Earth-sized planets in the habitable zones of Sun-like (LUMOS), and 4) a high-resolution UV spectropo- stars, measure their spectra, analyze the chemistry larimeter (POLLUX). LUVOIR covers a total band-

106 pass of 100 nm to 2500 nm and was designed to be The expected yield of potentially Earth-like planets serviceable and upgradable. We envision LUVOIR as is a critical metric for designing future exoplanet- a community-driven observatory, providing cutting- imaging missions. The fidelity of yield estimates edge scientific capabilities over a long mission life- has recently advanced dramatically and now include time. detailed instrument performance simulations, im- proved stellar catalogs, and additional sources of 301.14 — Observing the Solar System with background like solar glint and stray light from bina- LUVOIR: high angular resolution with a ries. Importantly, we now include all major sources segmented aperture of astrophysical noise, allowing us to provide ab- solute yield numbers with astrophysical uncertain- 1 1,2 Shawn Domagal-Goldman ; Roser Juanola-Parramon ; ties. Using these high-fidelity simulations, we con- 1 1 Giada Arney ; Aki Roberge firm previous results showing that exoEarth candi- 1 NASA Goddard Space Flight Center (Greenbelt, Maryland, date yield is a weak function of all mission and in- United States) strument parameters except for one: telescope aper- 2 University of Maryland - Baltimore County (Baltimore, Mary- ture. We show that obtaining a sample size for statis- land, United States) tical studies of directly-imaged potentially Earth-like planets requires a mission of the scale of LUVOIR. LUVOIR (Large UV Optical Infrared telescope) is a concept for a large multi-wavelength observatory, which would enable transformative advances across 301.16 — The LUVOIR Mission Concept: a broad range of astrophysics. With a proposed Technologies to Enable the Next Great launch date in the mid 2030s two architectures are Observatory being studied: LUVOIR-A (15-m) and LUVOIR-B (8- Matthew Ryan Bolcar1 m). In this presentation, we will review the Solar Sys- 1 Optics Branch / 551, NASA Goddard Space Flight Center (Green- tem observing capabilities of LUVOIR. belt, Maryland, United States) The High Definition Imager (HDI) instrument is the primary astronomical imaging instrument for The Large Ultraviolet/Optical/Infrared Surveyor observations in the near UV through the near IR. The (LUVOIR) is one of four mission concepts being stud- HDI design provides a 2 x 3 arcminute field-of-view, ied by NASA for the 2020 Decadal Survey in As- taking full advantage of the angular resolution pro- tronomy and Astrophysics. LUVOIR will be ca- vided by the telescope, and consists of two channels – pable of a broad range of science, including: di- UVIS (200 nm - 950 nm) and NIR (800 nm - 2500 nm). rect imaging and characterization of a wide range HDI would enable orbiter- and flyby-quality obser- of exoplanets and the search for biosignatures on vations of many solar system bodies, both large and Earth-like planets around sun-like stars; studying small. For instance, Pluto, which has a spatially het- galaxy formation and evolution; investigating star erogeneous surface, can be spatially and spectrally and planet formation; and remote sensing of bod- characterized with LUVOIR. LUVOIR could also ob- ies within the Solar System. Enabling a mission tain images of Jupiter with resolution comparable to as ambitious as LUVOIR requires an array of tech- the orbiter, and it could perform long-term nologies, such as ultra-stable structures and optics, monitoring of many outer solar system bodies that precision metrology and wavefront sensing, high- have not been visited by spacecrafts in recent decades contrast imaging techniques, large-format detectors (e.g. , Neptune) at high spatial resolution. with very low noise, and high-throughput ultravi- This poster will incluude simulated observations olet instrumentation. Critically, a systems-level ap- of Solar System bodies with the LUVOIR-A and proach must be taken to developing these technolo- LUVOIR-B instruments. It will compare such ob- gies, guided by architecture studies to place each servations with those from past, present and future technology in the appropriate system context. In space telescopes, using a conbination of real and sim- this poster, we describe LUVOIR’s technology needs, ulated observations. as well as current efforts that are actively develop- ing these technologies. We will discuss recent ad- 301.15 — Exoplanet Yield Estimates for the vancements in: measuring picometer-level displace- LUVOIR Mission Concept ments of optical and structural elements; sub-milli- kelvin thermal sensing and control; non-contact vi- 1 Christopher C. Stark bration isolation for pointing and dynamic stability; 1 Space Telescope Science Institute (Baltimore, Maryland, United coronagraph design for achieving 10−10 contrast on States)

107 a segmented system; high-speed metrology for op- transmission spectra and high spectral resolution, al- tical system alignment; low-order and out-of-band lowing us to detect transiting planetary exospheres wavefront sensing for maintaining high-contrast im- and constrain the physics of atmospheric escape. ages; low-noise detectors across the ultraviolet, op- Meanwhile, using the UVIS channel on the High Def- tical, and near infrared bands; broadband coatings inition Imager (HDI) instrument we can obtain high with high-reflectivity below Ly-α. We will also de- S/N R = 500 spectra in the optical and NUV, which scribe a systems approach to coordinating the devel- allow us to constrain the properties of clouds and opment of these technologies to achieve the neces- search for absorption from alkali metals. Finally, sary maturity for a LUVOIR mission start in the next with the NIR channel in HDI we will be able to detect decade. molecular absorption and measure abundances for a wide range of species including H2O, CO2, and O2. 301.17 — The State of the Wide-Field Camera 3 Russell E. Ryan1; Sylvia M. Baggett1; Matthew 302 — Solar Physics Division Bourque1; Gabriel Brammer1; Annalisa Calamida1; (SPD), Poster Session III Susana E. Deustua1; Harish G. Khandrika1; Jennifer Mack1; Myles McKay1; Norbert Pirzkal1; Elena Sabbi1; 302.01 — Formation and Eruption of Magnetic Ben Sunnquist1 Flux Ropes in the Solar Corona 1 STScI (Baltimore, Maryland, United States) Mark Linton1; Tibor Torok2; James Leake3 We will discuss the state of the Wide-Field Cam- 1 NRL (Washington, District of Columbia, United States) era 3 instrument on the Hubble Space Telescope. 2 Predictive Science Inc (San Diego, California, United States) In particular, we will describe our new implemen- 3 NASA Goddard (Greenbelt, Maryland, United States) tation for anomalous pixels and their effects in a new bad-pixel tables. In conjunction with that, we Magnetic flux ropes in the solar corona are often have implemented new time-dependent dark refer- thought to form the basis for both long-lived coro- ence images, which will be delievered to the archive. nal prominences and for eruptive coronal mass ejec- We will present analysis of the time-dependence of tions. In this presentation we discuss numerical sim- the photometric variability, photometric color terms, ulations exploring how such flux rope structures can and grism trace and dispersion recalibrations for the both be created and disrupted via the emergence UVIS detector. Finally, we provide suggestions, tips, of magnetic flux from the convection zone into the and recommendations for Users preparing Phase 2 corona. The presentation will focus on the formation files. of these structures directly from flux emergence as well as the effects, both stabilizing and eruptive, that 301.18 — Transmission Spectroscopy of newly emerging flux can have on pre-existing coro- Exoplanets with LUVOIR nal flux ropes.

1 1 1 This work is supported by the NASA Living with Eric Lopez ; Avi Mandell ; Daria Pidhorodetska ; Kevin a Star program and the Chief of Naval Research. France2 1 NASA GSFC (Greenbelt, Maryland, United States) 302.02 — (withdrawn) 2 CU Boulder (Boulder, Colorado, United States) This abstract was withdrawn. Transmission Spectroscopy is one of our most pow- erful tools for characterizing exoplanet atmospheres, 302.03 — NLTE inversions of Ca II 854.2 nm and thanks to the recent launch of NASA’s TESS mis- spectra from SOLIS/VSM: Temperature sion we will soon have a large sample of planets diagnostics around bright stars, ideally suited to this technique. With it’s unique combination of UV to NIR wave- Sanjay Gusain1; Christian Beck1 length coverage and incredibly high S/N, LUVOIR 1 National Solar Observatory (Tucson, Arizona, United States) would build upon the powerful legacy of Hubble and revolutionize our ability to characterize the at- We present non-local thermodynamic equilibrium mospheres of a wide range of transiting exoplanets. (NLTE) inversions of Ca II 854.2 nm spectra from SO- At FUV wavelengths the LUVOIR Ultravoilet Multi LIS/VSM observations. We show that precomputed Object Spectrograph (LUMOS) will obtain high S/N spectra from a database of model atmospheres can be

108 applied for a reliable inference of temperature strati- nal heating budget of these more complex waves and fications in the solar atmosphere. We show examples so provide a more complete lower boundary condi- of such inferences in different solar structures such tion for coronal and heliospheric models. as the umbra, penumbra, circum-facular regions and the quiet Sun. We also fit full Stokes profiles assum- 302.05 — Historical reconstruction of UV spectral ing a simple magnetic model with an exponential de- indices pendence with optical depth to derive vector mag- 1 2 2 netic field information and compare with the values Serena Criscuoli ; Francesco Berrilli ; Mia Lovric ; 2 derived from the weak-field approximation. Valentina Penza 1 National Solar Observatory (Boulder, Colorado, United States) 2 302.04 — Preparing for DKIST: Connecting the University of Rome TorVergata (Rome, Italy) High-Resolution Sun to the Turbulent Corona Solar radiation is one of the major natural drivers Samuel Van Kooten1; Steven R. Cranmer1 of Earth climate changes observed from the Maun- 1 Astrophysical & Planetary Sciences, University of Colorado, der minimum. UV radiation in particular plays a Boulder (Boulder, Colorado, United States) major role in the ozone production/destruction pro- cesses and is known to affect the circulation patterns. Magnetic bright points on the solar photosphere, vis- Here we present reconstructions of the FUV-MUV ible in both continuum and G-band images, indicate and CaII and MgII core-to-wing indeces footpoints of kilogauss magnetic flux tubes extend- from 1749-2015, performed with a semi-epirical ap- ing to the corona. The horizontal motions of these proach. We also present a reconstruction of the TSI footpoints are believed to excite MHD waves which variability. Our results are compared with recon- propagate to the corona, where they deposit heat structions obtained with models employed in clima- through turbulent dissipation. Analyzing this mo- tological studies. tion can thus provide a power spectrum of MHD wave energy transport, which is a key lower bound- 302.06 — What do we reliably know about how ary condition in coronal and heliospheric models. At fast the Sun’s core spins? ∼100 km in diameter, most bright points are seen as unresolved blobs. Tracking their centroids al- Philip H. Scherrer1; Douglas Gough2 lows the excitation of kink-mode waves to be mod- 1 Stanford Univ. (Stanford, California, United States) eled in the overlying flux tubes. However, centroid 2 University of Cambridge (Cambridge, United Kingdom) tracking cannot easily handle the merging or split- ting of bright points nor can it track extremely long Fossat et al. (2017) and Fossat & Schmider (2018) bright points, and current observations cannot re- have attempted to use solar p-mode frequency per- veal more complicated motions, such as size or shape turbations to detect rotational splitting of g-modes. changes, which are expected to excite higher-order They claim that this approach detected the Sun’s waves. DKIST promises to resolve the sizes and core to be rotating about 3.8 times faster than the shapes of bright points. However, Agrawal et al. surrounding radiative interior and the convection (2018) showed that centroid tracking is likely to ex- zone. We report an independent study of the tech- perience a spurious ”jitter” signal when applied to nique, the inconsistencies with the well-established high-resolution data, and this limitation is in addi- p-mode determinations of rotation, and with their tion to the inability of centroid tracking to produce assumption of which g-modes might be sensed. Ad- new insights from the new size and shape informa- ditionally we used both the same calibrated 80s tion. We present efforts to overcome these limita- SOHO/GOLF data used in the 2017 study and the tions by developing an algorithm to infer the hor- then only publically available GOLF 60s cadence izontal plasma flow inside bright points at DKIST- data and verified the findings of Schunker etal. like resolution (at which bright points are resolved (2018) that the g-mode detection was fragile: It van- but not large enough for traditional correlation- ished when the GOLF data was sampled at the 60s tracking techniques) and using these inferred flows vs 80s cadence and when the starting point was to model the higher-order waves generated in the shifted by 2 hours of the 15 years studied. We also overlying flux tubes. By using output data from applied the same technique to all other available high-resolution MURaM simulations now, we expect long duration low-degree data collections including to be prepared to analyze DKIST images soon after SOHO/MDI, SOHO/LOI, SDO/HMI, GONG, and they become available next year. This work will esti- BiSON and found no evidence of the Fossat et al. mate the significance of the contribution to the coro-

109 (2017) reported signals. We note that a second in- The 3D Global solar convection algorithm EULAG- dependent study by Appourchaux & Corbard (2019) MHD has recently been used to recreate solar hydro- came to the same conclusions. Thus we doubt the va- dynamic profiles of differential rotation and merid- lidity of the 2017 findings and conclude that there is ional circulation along with simulation of long-term no useful information about the rotation of the solar evolution of the global magnetic field. In previ- core yet determined using these techniques (Scher- ous studies we saw some of the large effects that rer & Gough, 2019). References: Appourchaux, T., are created by including strong shear layers in the & Corbard, T. 2019, Submitted to A&A, Fossat, E., tachocline and on the surface; changing the period Boumier, P., Corbard, T., et al. 2017, A&A, 604, A40, of the solar cycle from an order of years to that of Fossat, E., & Schmider, F. X. 2018, A&A, 612, L1, decades. We attempt to explore the global conse- Scherrer, P. & Gough, D., Accepted by ApJ, 2019, quences of these regions by simulating various lev- Schunker, H., Schou, J., Gaulme, P., & Gizon, L. 2018, els of sub/super-adiabaticity in the background po- SoPh, 293, 95 tential temperature profiles – modeled by a poly- tropic with manually controlled polytropic 302.07 — Temporal Evolution of the Sun’s Interior indeces, simulating the creation or suppression of Meridional Circulation during 2010 — 2018 a near-surface shear layer (NSSL). We also attempt to understand how the MPDATA algorithm that is 1 1 Ruizhu Chen ; Junwei Zhao implemented in the model will function under var- 1 Stanford University (Stanford, California, United States) ious resolutions (512 φ, 256 θ, 256 R; 256 φ, 128 θ, 128 R) where an implicit viscous dissipation is im- The Sun’s meridional circulation plays an impor- plemented using the implicit Large-Eddy simulation tant role in solar dynamo, which drives the Sun’s (ILES) approach for turbulent advective motions – a magnetic-field variation cycles, and it is curious method that can be unpredictable as large changes how the meridional circulation itself evolves with in resolution begin to change scales of dissipation in the solar cycle. In this study, we employ a newly- low viscosity environments. The simulation of our developed comprehensive time-distance helioseis- NSSL is done at a lower resolution (128 φ, 64 θ, 64 R) mic measurement scheme, make measurements us- that has repeatedly been shown to adequately sim- ing SDO/HMI Doppler-velocity observations from ulate solar-like hydrodynamic effects such as differ- 2010 to 2018, and explore the temporal evolution ential rotation, as well as generate well defined cycli- of the meridional circulation over different phases cal magnetic dynamo patterns. These models show of the current solar cycle. Our new measurement the NSSL as playing an important role in the proper method measures acoustic travel-time shifts along distribution of angular momentum and resulting in all radial directions of the solar disk for all possi- more realistic solar-like magnetic and hydrodynamic ble measurement distances, and removes the system- patterns. atic center-to-limb effect through solving a set of lin- ear equations. Measurements are made on every 302.09 — Time-Dependent Hydrodynamic two-year data chunk to obtain the time-dependent Modeling of Solar Acoustic Waves meridional-flow-induced travel-time shifts, which show a significant change between the solar activity John Stefan1; Alexander G. Kosovichev1 minimum and maximum. The travel-time shifts are 1 New Jersey Institute of Technology (North Brunswick, New Jersey, then inverted for meridional flow in a least-square United States) way. We show evidence of temporal variation of the meridional-circulation pattern over different phases We consider linear perturbations to appropriate hy- of the cycle. drodynamic equations, such as mass continuity and the adiabatic condition. Using the Solar Model S (Christensen-Dalsgaard 1996- 2014) as mesh, we dis- 302.08 — Modeling of Subsurface Shear with cretize the governing equations as well as decom- EULAG-MHD pose the various modes using spherical harmonics. Andrey Maksimovich Stejko1; Gustavo Guerrero2; We take advantage of parallel computing resources Alexander G. Kosovichev1 by running simulations up to very high modes of or- 1 Physics, New Jersey Institute of Technology (Jersey City, New der l=3000. This allows us to model so-called “sun- Jersey, United States) quakes” with fairly high precision; since the govern- 2 Physics, Federal Institute of Minas Gerais (Belo Horizante, Minas ing equations allow for different types of perturba- Gerais, Brazil) tions, we aim to determine the location and mecha- nism of these impulsive events.

110 302.10 — Active Region Flows and their the CoMP telescope providing information about Contribution to Varying Global Dynamics coronal magnetic direction and topology. Other observations such as linear polarization in UV un- Douglas Braun1 1 saturated Hanle measurements provide important NWRA (Boulder, Colorado, United States) complementary information about the strength of 3D coronal field. Until such observations are avail- We explore the general properties of the near-surface able, we turn to the FORWARD model (Gibson et dynamics of solar active regions (ARs) and show al. 2016) to explore how these polarization data how AR flows may contribute to longitudinally might be used together to interpret the coronal mag- averaged measurements of global properties such netic field. As a physical state to input into FOR- as meridional circulation and torsional oscillations. WARD, the analytic magnetic model in this work is Helioseismic holography is applied to HMI Dopp- adopted from Gibson et al.(1996), which is an ax- lergrams yielding about 5000 flow measurements of isymmetric model and gives a potential field with 336 ARs observed by SDO between 2010 and 2014. an exception at the boundary of the Ensemble averages of the AR flows are presented, where current sheets are added between the open binned into subsets based on total magnetic flux. and closed fields. The plasma model is adopted These averages show converging flows, with speeds from Sittler&Guhathakurta (1999) and Vásquez et al. about 10 m/s and spanning 10 degrees from the (2003), which is consistent with multi-observations. active region centers, which are apparent for most Given this model input of a 3D distribution of mag- ARs above the flux limit of our survey at 1021 Mx. netic field and plasma for , we obtain Retrograde flows are also detected, with amplitudes simulated polarization results in UV and visible/IR around 10 m/s, which predominantly, but not ex- wavelengths. This allows us to consider how such clusively, flank the polar side of the ARs. The high observations might be used together in future to di- signal-to-noise levels of these averages makes possi- agnose the coronal magnetic field. ble the assessment of individual AR contributions to time-varying global flows. We demonstrate this for several solar rotations, showing that individual ac- 302.13 — Retrieving 3D coronal magnetic field tive regions contribute substantially to these global from ground and space based spectropolarimetric flows. observations This work is supported by the Solar Terrestrial Maxim Kramar1; Haosheng Lin1 program of the National Science Foundation (award 1 University of Hawaii at Manoa (Pukalani, Hawaii, United States) AGS-1623844) and by the NASA Heliophysics Divi- sion (awards 80NSSC18K0066 and 80NSSC18K0068). Solar coronal magnetic fields play a key role in the energetics and dynamics of coronal heating, solar 302.11 — (withdrawn) wind, solar flares, coronal mass ejections (CME), filament eruptions, and determine space weather This abstract was withdrawn. processes. Therefore, precise knowledge of the 3D magnetic field and thermodynamic structures of the 302.12 — Spectropolarimetric diagnostics of corona is essential for the heliophysics community’s coronal magnetic field from UV and visible/IR effort to understand the physics of the solar wind during solar minimum and solar eruptive phenomena. With the recent ad-

1 2 3 vancement of scalar and vector tomographic inver- Jie Zhao ; Sarah Gibson ; Silvano Fineschi ; Roberto sion techniques (Kramar et al., 2016), it is now possi- Susino3 1 ble to directly derive the 3D coronal magnetic, tem- Purple Mountain Observatory, CAS (Boulder, Colorado, United perature, and electron density structures using syn- States) 2 optic Fe XIII 1075 nm coronal emission line (CEL) High Altitude Observatory, NCAR (Boulder, Colorado, United linear polarization data of the Coronal Multichannel States) 3 Polarimeter (CoMP, Tomczyk et al., 2008), and UV Turin Astrophysical Observatory, INAF (Turin, Italy) coronal images from STEREO mission. This is a ma- jor milestone in our effort to establish the capabilities The invisible magnetic field in the corona plays an to directly observe 3D magnetic and thermodynamic important role for solar activity, hence measuring structures of the corona. the coronal magnetic field is highly desired. The Although the vector tomography based on lin- linear polarization measurements in the saturated ear polarization (LP) data can be used to probe cer- Hanle regime of visible/IR are already obtained by tain coronal field configuration (Kramar et al. 2013),

111 linear polarization data alone does not allow us to linear polarization produced by scattering processes uniquely reconstruct all possible field configurations in the hydrogen Lyman-α line of the solar disk ra- in general. In the near future, the arrival of DKIST diation. The analysis and interpretation of such will provide the multi-CEL full-Stokes data more ac- spectro-polarimetric observation allowed us to ob- curate determination of the static corona using the tain information on the geometrical complexity of rotation of the Sun to emulate tomographic observa- the corrugated surface that delineates the TR, as well tions. as on the magnetic field strength via the Hanle ef- On the longer term, observational determination fect. At the same time, the CLASP slit-jaw (SJ) op- of spatially and temporally resolved B(r; t), T(r; t), tics system, which is a Lyman-α filter imager char- and n(r; t) will require the deployment of a Space acterized by a FWHM= 7 nm, allowed us to obtain Coronal Magnetometry Mission (SCMM) with a fleet broad-band Stokes-I and Q/I images over a large of spacecraft observing the Sun from many non- field of view. The obtained broad-band Q/I im- redundant circumsolar orbits simultaneously. ages are dominated by the scattering polarization We will discuss how the use of full Stokes polariza- signals of the Lyman-α wings, and not by the much tion data and multiple observing geometry from and weaker line-center signals where the Hanle effect op- out of the ecliptic plane will improve the accuracy of erates. Recently, Alsina Ballester et al. (2019, ApJ, coronal magnetic field reconstruction. in press) showed that the scattering polarization sig- nals of the Lyman-α wings are sensitive to chromo- 302.15 — Idealized MHD Simulations of spheric magnetic fields via the magneto-optical ef- Eruptions in the Solar Atmosphere fects. Therefore, Lyman-α imaging polarimetry is of scientific interest also for magnetic-field inves- 1 James E. Leake tigations. On April 11, 2019, we performed an- 1 NASA Goddard Space Flight Cemter (Alexandria, Virginia, other sounding rocket experiment, called the Chro- United States) mospheric LAyer Spectro-Polarimeter (CLASP2). We used the same instrument after significant modifica- We present a parameter study of numerical simu- tions in order to obtain spectro-polarimetric obser- lation designed to explain the onset of major solar vations of a plage and a quiet region in the ionized eruptions from solar active regions. We investigate magnesium lines around 280 nm (i.e., the Mg II h & the likelihood of eruption based on the emerging k lines). At the same time, the CLASP2 SJ optics sys- magnetic flux and the pre-existing flux. tem allowed us to obtain broad-band Q/I and U/I images at the Lyman-α wavelength, in addition to 302.16 — Lyman-α imaging polarimetry with the the well-known SJ intensity images. In this presen- CLASP2 sounding rocket mission tation, we provide a first overview of the CLASP2 SJ data. Ryouhei Kano1; Ryohko Ishikawa1; David Eugene McKenzie2; Javier Trujillo Bueno3; Donguk Song1; Masaki Yoshida1,4; Takenori Okamoto1; Laurel 303 — Stars & Stellar Evolution Rachmeler2; Ken Kobayashi2; Frederic Auchere5 1 National Astronomical Observatory of Japan (Tokyo, Japan) Poster Session 2 NASA Marshall Space Flight Center (Huntsville, Alabama, United States) 303.01 — Fundamental Stellar Parameters and 3 Instituto Astrofisica de Canarias (Santa Cruz de Tenerife, Spain) Multiplicity Rates of M-Dwarfs through Optical 4 The Graduate University for Advanced Studies (Sokendai) (Kana- Speckle and NIR AO Imaging gawa, Japan) Frederick Hahne1; Elliott Horch1; David R. Ciardi6; Ger- 5 Institut d’Astrophysique Spatiale (Paris, France) ard van Belle5; Catherine Clark2; Jennifer Winters4; Todd J. Henry3 Ultraviolet polarimetry offers a unique opportunity 1 to explore the upper solar chromosphere and the Department of Physics, Southern Connecticut State University (New Haven, Connecticut, United States) transition region (TR) to the million-degree corona. 2 These outer atmospheric regions play a key role in Northern Arizona University (Flagstaff, Arizona, United States) 3 RECONS Institute (Chambersburg, Pennsylvania, United States) the transfer of mass and energy from the solar pho- 4 tosphere to the corona. With a sounding rocket ex- Harvard University (Cambridge, Massachusetts, United States) 5 Lowell Observatory (Flagstaff, Arizona, United States) periment called the Chromospheric Lyman-Alpha 6 Spectro-Polarimeter (CLASP), in September 2015 we California Institute of Technology (Pasadena, California, United succeeded in obtaining the first measurement of the States)

112 We present preliminary fundamental stellar param- 2 University of Illinois (Champaign-Urbana, Illinois, United States) eters and multiplicity rates of M dwarf stars us- ing a combination of speckle imaging and adap- Galactic extinction complicates the study of many of tive optics. Our survey mainly uses the Differential the most massive stars in our own galaxy. Surveys Speckle Survey Instrument (DSSI) at Lowell Obser- of luminous stars in nearby galaxies contain many vatory’s Discovery Channel Telescope (DCT). DSSI massive stars but those surveys must contend with observes speckle patterns simultaneously at two sep- the misidentification of dwarfs and AGB stars as su- arate wavelengths and the data for this project are pergiants (foreground contamination). Massey et al. composed of observations which span from 2016 to (2009) built a list of several hundred M31 red super- 2018. More recently, the speckle data for some of the giants (RSG) using color-color photometry and later target stars that have been found to be binary have Massey & Evans (2016) used radial velocities to fur- been supplemented with observations using Adap- ther refine that list. We have cross-correlated those tive Optics (AO) at Palomar Observatory. The com- lists with high precision parallaxes from Gaia DR2 bination of speckle data in the visible and AO data in order to determine the utility of Gaia parallaxes in the near-infrared allows us to make robust deter- for distinguishing foreground sources and RSG and minations of the luminosities and effective temper- M31. atures of the components in each case. Using the known Mass-Luminosity Relation, we also estimate 303.04 — The PolStar SMEX Mission — Science the component masses. A discussion of interesting Drivers and Scope systems will be given. Paul A. Scowen1 1 Arizona State Univ. (Tempe, Arizona, United States) 303.02 — Update on a Survey of the Most Luminous Stars in M31 and M33 PolStar is a FUV spectropolarimeter SMEX mission John C. Martin1 that is the first to combine the spectroscopic capabil- 1 Chemistry, U of Illinois Springfield (Springfield, Illinois, United ities previously available in IUE and HST-COS with States) the polarimetric capabilities of a true successor to WUPPE. PolStar will provide access to the suite of Post-main sequence evolution of the most luminous resonance lines in the FUV to map the wind and stars significantly contributes to the chemical enrich- magnetospheric structure of massive stars in 3D and ment history of the universe. They also provide in- gain insight into the effect these structures have on sight to extreme physics and unexplained eruptive the mass loss and stellar evolution of the stars them- behavior (i.e. supernova impostors and S Doradus selves. The mission will also address science related eruptions) which are not normally predicted by stel- to how massive binary pairs interact with each other, lar modeling. Unfortunately, because there are not as and provide access to the interstellar reddening law many to study, the later stages of massive star evolu- at very short wavelengths for a variety of sight lines. tion are not as well observed and understood as the The suite of science drivers is discussed in terms of evolution of low mass stars. Heavy extinction in the requirements placed on the mission design and we plane our own galaxy makes the luminous/massive outline the kinds of return we might expect from this star populations in nearby galaxies easier observe at mission, if selected. shorter wavelengths (where they emit most of their energy). Since 2012 we have monitored brightness 303.05 — Simulating the Inner Asterospheric changes of the most luminous stars in M31 and M33 Magnetic Fields of Exoplanet Host Stars with a targeted survey focused on luminous blue 1 1 2 variables (LBV), candidate LBV, B[e] supergiants, Alison Farrish ; David Alexander ; Mei Maruo ; An- 1 1 3 and warm hypergiants. We report on the progress of thony Sciola ; Frank Toffoletto ; Marc L. DeRosa 1 this survey, focusing on trends emerging in the vari- Physics and Astronomy, Rice University (Houston, Texas, United ability of the different classes of massive stars within States) 2 the classifications studied. Kyoto University (Kyoto, Japan) 3 Lockheed Martin (Palo Alto, California, United States) 303.03 — Using Gaia Parallaxes to Distinguish We study magnetic and energetic activity across a M31 Red Supergiants from Foreground Stars range of stellar behavior via the application of an Logan Michael Kimball2; John C. Martin1 observationally-based heliophysics modeling frame- 1 U of Illinois Springfield (Springfield, Illinois, United States) work. We simulate the inner asterospheric magnetic

113 fields of host stars with the aim of better under- observations during that time. It also confirms the standing and constraining the space weather envi- chromatic nature of these events, suggesting that the ronments of exoplanets, and improving our knowl- material obstructing the stars light is optically thin. edge of the solar-stellar connection. As astronomy Additionally, the secular dimming has not been wit- instrumentation has improved, Earth-like exoplan- nessed and conversely, the star has portrayed a slight ets are increasingly being found orbiting in the hab- rising trend over this period. itable zones of a variety of stars, ranging from the smallest and coolest M dwarfs to larger and more 303.07 — Developing a Python Package for solar-like stars. We are therefore interested in char- Automated Mineralogical Compositional Analysis acterizing a broad range of stellar magnetic activity 1 1 and the resulting impacts on asterospheric environ- Yung Kipreos ; Inseok Song 1 ments. We will present our work simulating stellar Physics & Astronomy, The University of Georgia (Athens, Geor- magnetic activity on cycle timescales via the integra- gia, United States) tion of modeled magnetic flux emergence, coronal The circumstellar disk that surrounds a star is com- field structure and related plasma emission, and stel- posed of the gas and dust particles that are in orbit lar winds. We use this self-consistent framework of around it. Around infant stars, this disk can act as a heliophysics-based models to simulate stellar and as- source of material that can be used to form planetesi- terospheric evolution, in order to better understand mals, which can then accrete more material and form the dynamic connections between host stars and po- into planets. The composition of these circumstel- tential impacts on planetary space weather and hab- lar disks is of importance because it can indicate ei- itability. We also remark on the comparative helio- ther what future are likely to be made physics approach which we plan to extend to star- of, or it can shed some light on the history of any planet interactions via coupling to models of mag- planetesimals that have already formed. In this re- netospheric activity and dynamo-driven stellar flux search project, we have created an automated com- emergence. puter program that will take in the spectra of a cir- cumstellar disk as input and will output its most 303.06 — Automated Pipeline for the Continuous likely mineral composition and the relative abun- Monitoring of KIC 8462852 Using the Great Basin dances of each mineral. For the mineral spectra, we Observatory used the mid-infrared wavelength range because the Jacob Fausett1,2; Jonathan Swift3; Melodi Rodrigue1,2 inner section of the circumstellar disk, where plan- 1 Physics, University of Nevada, Reno (Sparks, Nevada, United etesimals are thought to form, radiates strongest in States) mid-infrared light. The most likely mineral compo- 2 Great Basin Observatory (Baker, Nevada, United States) sition is found by using the linear least square mini- 3 The Thacher School (Ojai, California, United States) mization method on the observed circumstellar spec- tra data. The creation of this program will help to KIC 8462852 has puzzled astronomers since its ape- identify the possible mineral composition at a faster riodic fluctuations in brightness and long- term sec- rate than could be done otherwise. The final mineral ular dimming was discovered in 2016. Based on that compositional analysis result can then be compared initial data from the Kepler mission, an international to various solar system objects such as comets and collaboration has sought to better understand these asteroids. two phenomena. Over the past three years, a net- work of observatories has been monitoring the star 303.08 — BVRcIc Observations and Analysis of the nightly in order to see these fluctuations in real time Totally Eclipsing Very Short Period Algol Binary, and send alerts to the community for further obser- V385 Camelopardalis vation. The research presented here is in an effort to contribute to the continuous monitoring of KIC Ronald G. Samec1; Daniel B. Caton2,3; Danny R. 8462852 using the Great Basin Observatory. Nightly Faulkner4 observations are scheduled with ACP Observatory 1 Pisgah Astronomical Research Institute (Hartwell, Georgia, Control Software and an automated pipeline, using United States) Python’sAstropy and IRAF has been set up to pro- 2 Appalachian State University (Boone, North Carolina, United cess the images and perform photometry in order States) to quickly recognize a dimming event. Since March 3 Dark Sky Observatory (Boone, North Carolina, United States) of 2018, our data show the largest such event since 4 University of South Carolina (Lancaster, South Carolina, United the initial Kepler data and is consistent with other States)

114 V385 Cam is a F5V±2 type (T∼ 6500K) eclipsing bi- 4 Johnson Observatory, 1414 Bur Oak Court, Hebron, KY 41048 nary. It was observed on December 15, 16, 17, and (Hebron, Kentucky, United States) 18, 2017 at Dark Sky Observatory in North Carolina with the 0.81-m reflector of Appalachian State Uni- AE Cas was observed some 40 years ago by Srivas- versity. Three times of minimum light were deter- tava and Kandpal (1984) and analyzed by a Fourier mined from our present observations, which include technique. This study represents the first modern two primary eclipses and one secondary eclipse: synthetic analysis of light curves using the 2015 ver- HJD Min I = 2457372.62072 ± 0.00034, 2457374.4578 sion of the Wilson-Devinney Program. V, Rc,Ic ± 0.0042, HJD Min II = 2457372.9266 ± 0.0011. In observations were taken October 3, 4 and 23, 2016 addition, an ephemeris was given by Shaw, https: at Dark Sky Observatory in North Carolina with //www.physast.uga.edu/~jss/ncb/. Other times the 0.81-m reflector of Appalachian State Univer- of minima were given in BRNO and Diethelm 2013, sity and remotely by the 0.9-m reflector at KPNO An ephemeris was calculated by ASAS-SN, https: from the SARA consortia. Five times of minimum //asas-sn.osu.edu/: JD Hel Min I 2457386.76033 + light were determined from our present observa- 0.6152709 × E. Eight times of low light were calcu- tions, which include three primary eclipses and lated using least squares fits to archived data from two secondary eclipses: HJD Min I = 2457663.5055 asas. The following quadratic ephemeris was deter- ± 0.0005, 2457684.76093 ± 0.00005, 2457684.7616 ± mined from the available times of minimum light: 0.0001; HJD Min II = 2457663.8843 ± 0.0006 and JD Hel Min I = (245157372.61838 ± 0.00063) d + 2457664.652. In addition, eight observations at min- (0.61527012 ± 0.00000077) × E - (0.00000000014 ± ima were introduced as low weighted times of min- 0.00000000008) × E2. imum light taken from archived ASAS data and 74 The weak period decrease may indicate that the times of minimum light from the literature, some be- mass is flowing from the secondary Lagrangian ing from visual observations. The following linear and quadratic ephemerides were determined from point to the primary component. BVRcIc simultane- ous 2015 Wilson-Devinney Program (W-D) solutions all available times of minimum light: JD Hel Min I = gives a mode 5 classical Algol solution (secondary (2457684.7640 ± 0.0009) d + (0.75912076 ± 0.00000006) component filling its Roche Lobe, primary under- × E, JD Hel Min I = (2457684.75610 ± 0.00085) d + (0.75911881 ± 0.00000014) × E - (0.000000000047 ± filling). The semidetached solution gives a primary 2 component with a 93% fill-out. The solution gives a 0.000000000003) × E . The period decrease may indi- mass ratio of 0.2808 ± 0.0057, and a component tem- cate the binary is undergoing magnetic braking and perature difference of ∼1500 K. The large ΔT in the is approaching contact configuration. Otherwise, the components verify that the binary is not yet in con- near contact secondary component may be stream- tact. A Binary Maker fitted dark spot did not persist ing matter onto the primary, more massive compo- in the WD Synthetic Light Curve Computations even nent. A BVRcIc simultaneous Wilson-Devinney Pro- though there is a definite asymmetry at phase ∼0.75. gram (W-D) preliminary solution indicates the possi- The inclination is ∼83.1 ± 0.3 degrees, resulting in a bility that the system has a mass ratio somewhat less total eclipse (secondary component) of 16.3 minutes than unity (q = 0.856 ± 0.001), and a component tem- in duration. The system’s distance is 854 (±13) pc as perature difference of ∼2060 K. The large ΔT in the determined from GAIA DR2. Additional and more components verifies that the binary is not yet in con- detailed information is given in this report. tact. No spots were needed for the solution, so if the stream exists it is week as verified by the small period decrease. Fill-out of our model is 83.2% for the pri- 303.09 — Observations and Modern Light Curve mary component and 99.1% for the secondary com- Analysis of the Detached Solar Type Binary, AE ponent. The inclination is ∼76°, not enough for the Cas system to undergo a total eclipse. The light curve in Heather Chamberlain1; Dr. Ronald Samec2; Daniel B. V is more than one magnitude in amplitude. Addi- Caton3; Danny R. Faulkner4 tional and more detailed information is given in this 1 Pisgah Astronomical Research Institute (Hartwell, Georgia, report. United States) 2 Faculty Research Associate, Pisgah Astronomical Research In- 303.10 — Constraining Tidal Dissipation in stitute, 112 Idlewood Acres, Hartwell, GA 30643 (Hartwell, Georgia, Low-mass Binary Systems United States) Ruskin Patel1; Kaloyan Penev1 3 Dark Sky Observatory, Applachian State University, Department 1 Physics, University of Texas at Dallas (Dallas, Texas, United of Physics and Astronomy (Boone, North Carolina, United States) States)

115 Tidal interactions are known to drive the orbital evo- joint light curve and radial velocity solution, includ- lutions in binary systems. As a result, the current ing multi-year photometry from LCOGT, SkyMap- rotation period of the primary star and the orbital ec- per and TESS, combined with spectroscopy from centricity in the system depend upon the tidal dissi- Magelland/MIKE and the ANU 2.3-m/WiFeS spec- pation efficiency in stars. The most widely accepted trograph. The observations and modelling yield model is to assume a phase lag in the tidal bulge with components of 0.5 and 0.2 solar masses, with radii in respect to companion raising tides on the star. This good agreement with 25 Myr isochrones and mem- phase lag is parameterized as Tidal Quality Factor bership in 32 Orionis. Straddling the 0.35 solar mass (Q) which qualitatively determines the energy lost fully-convective boundary for M dwarfs, the sys- in a system due to tides. In this study, we use ob- tem is uniquely placed to test models of low-mass served rotation periods of the stars and orbital eccen- star formation, structure and evolution at interme- tricities in several low mass Kepler binaries to con- diate epochs between the youngest star-forming re- straint Q by running MCMC simulations. I present gions and older open clusters like Praesepe and the here the stellar and orbital evolution model used and , where several new low-mass eclipsing sys- the results and analysis of the simulations for a few tems have recently been found in K2 photometry. of these systems. This study is aimed towards us- ing a large number of binaries in order to explore the 303.12 — A Photometric Study of RR Lyrae Star dependence of Q upon various observational param- TU UMa eters. Kristen L. Thompson1; Jamie Barnhill1; Caroline Evans1; 1 1 303.11 — A 25 Myr-old M+M eclipsing binary Andrew Fay ; Meg Houck 1 spanning the fully-convective boundary Davidson College (Cornelius, North Carolina, United States) Simon J. Murphy1,2; Eric E. Mamajek3; Cameron P.M. RR Lyrae stars are short-period, pulsating variable Bell4; Warrick Lawson1; Michael S. Bessell2; Christopher stars that are useful for determining cosmic dis- A. Onken2; David Yong2; Gary S. Da Costa2; George tances. The goal of this investigation is to ana- Zhou5 lyze photometric data of TU UMa, a variable star of 1 School of Science, University of New South Wales Canberra (Can- RR Lyrae type, for distance determination. A com- berra, Australian Capital Territory, Australia) prehensive light curve was constructed from peri- 2 Australian National University (Canberra, Australian Capital odic optical observations using the Las Cumbres Ob- Territory, Australia) servatory telescope network over the course of two 3 Jet Propulsion Laboratory, California Institute of Technology weeks. The B, V, i, and Z filters were used and expo- (Pasadena, California, United States) sure times were adjusted for each filter. TU UMa has 4 Leibniz Institute for Astrophysics Potsdam (AIP) (Potsdam, Ger- been studied extensively for about a century due to many) its status as the best candidate for an RR Lyrae star in 5 Center for Astrophysics, Harvard (Cambridge, Massachusetts, a binary system. This project is part of a larger collab- United States) oration to study a set of RR Lyrae stars. Preliminary results will be discussed. Although M dwarfs comprise the majority of stars in the Galaxy, a detailed understanding of these ubiq- 303.13 — Exploration of Compact Binary Systems uitous objects remains elusive. For example, current Using Empirical Gaia Photometry modelling struggles to accurately predict masses and radii in M dwarfs and this is especially true of pre- Isaac Daniel Lopez1; JJ Hermes1 main sequence systems, where evolutionary mod- 1 Astronomy, Boston University (Allston, Massachusetts, United els are poorly constrained observationally. Double- States) lined eclipsing binaries are key yardsticks for funda- mental stellar parameters. However, due to the in- We explore Gaia DR2 for new compact binary sys- trinsic faintness of such systems, there are currently tems within 200 parsecs using a method based on re- only a few dozen M+M eclipsing binaries that can ported mean G band flux uncertainties. More vari- be used to robustly test models and only a hand- able objects should have larger empirical photomet- ful of suitable pre-main sequence systems. We have ric uncertainties. A preliminary list of candidate ob- recently identified and fully characterised a young jects has been cross matched to known compact bi- (25 Myr), nearby (103 pc) eclipsing binary which is naries. The next step in this work is to obtain follow- a member of the under-studied equatorial moving up high-speed photometry of the objects that were group 32 Orionis. We present the results of our unknown before Gaia DR2. Follow-up observations

116 will allow us to determine what kind of objects, if tangling analysis we also precisely measured the ra- any, are preferentially selected by this method. Test- dial velocity variations of both stars using HET HRS ing the reliability of this method for selecting candi- spectra. Together these measurements allow us to date objects will be important for future Gaia data determine the mass and radius of each star. We find releases. that the primary star has M1=1.76 M⊙ and R1=2.20 R⊙, while the secondary star has M2=1.22 M⊙ and 303.14 — Modeling the Evolution of Type IIb R2=1.20 R⊙. In the color-magnitude diagram of the Supernovae in a Binary Circumstellar Medium cluster, the primary star is located at the main se- quence turnoff where it is beginning rapid changes 1 1 Christopher Kolb ; Stephen P. Reynolds ; Kazimierz J. after its core hydrogen burning phase. By using the 1 1 Borkowski ; John M. Blondin rapid radius change of the more massive star, we will 1 Physics, North Carolina State University (Raleigh, North Car- determine an accurate age for the cluster using the- olina, United States) oretical stellar models. We gratefully acknowledge support from the NSF under grant AST-1817217. The presence of slow, dense stellar wind in binary systems can produce a highly asymmetric circum- 303.16 — The K2 M67 Study: Star Masses in an stellar medium (CSM), particularly for systems with Old from a New Eclipsing Binary a mass outflow velocity comparable to the binary’s orbital velocity. Mass loss in such a system is signif- Eric L. Sandquist1; David W. Latham8; Robert D. icantly enhanced in the equatorial plane, with a re- Mathieu2; Emily Leiner3; Andrew Vanderburg4; sulting polar-to-equatorial density contrast of 10 to Luigi R. Bedin5; Mattia Libralato7; Luca Malavolta6; ∼300. We aim to better understand this asymmet- Domenico Nardiello6; Jerome A. Orosz1 ric CSM in the context of supernovae IIb progenitors 1 San Diego State Univ. (San Diego, California, United States) and to study the impact on supernova morphology 2 University of Wisconsin - Madison (Madison, Wisconsin, United and resulting observational signatures. States) We model the asymmetric wind and subsequent 3 Northwestern University (Evanston, Illinois, United States) supernova explosion with full 3D hydrodynam- 4 University of Texas - Austin (Austin, Texas, United States) ics using the shock-capturing hydro code VH-1 5 Istituto Nazionale di Astrofisica (Padova, Italy) on a spherical yin-yang grid. We investigate a 6 University of Padova (Padova, Italy) range of CSM parameters including companion-to- 7 Space Telescope Science Institute (Baltimore, Maryland, United primary mass ratios spanning 0.7-2.5, asymptotic States) wind speeds between 15-25 km/s, and orbital-to- 8 Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- wind velocity ratios ranging 1.0-2.0. For each, the re- sachusetts, United States) sulting CSM is used to evolve a blastwave out to a few tens of years. In some cases, the blastwave remains We analyze Kepler K2 photometry and ground-based quite asymmetric for years, maintaining a polar-to- radial velocities for the binary Sanders 617. This equatorial radius ratio >2.5. We discuss this mor- eccentric binary was discovered to have only one phology and the observational implications of the re- eclipse per 62.595 d orbital cycle, but because of the sulting data, with a focus on radio brightness from a long period, the inclination of the binary and the few weeks to months. stellar masses are tightly constrained. Because there is an extensive literature of M67 photometry from 303.15 — Age of the Open Cluster NGC 752 from the ultraviolet to the infrared, we have developed a the Eclipcing Binary DS And. method to use the spectral energy distributions of cluster members to decompose the light of the bi- 1 1 Andrew John Buckner ; Eric L. Sandquist ; Matthew D. nary into single cluster stars. The primary star has Shetrone2; Jerome A. Orosz1 a mass of 1.22 M⊙ and resides at the lower turnoff 1 Astronomy, San Diego State University (San Diego, California, (the fainter of two maximums in Teff) for the clus- United States) ter. While models are able to match the masses and 2 University of Texas at Austin (Austin, Texas, United States) photometry of the fainter star in the binary and solar analogs in the cluster, the brighter star in the binary We present a new analysis of the 1.01-day period is significantly fainter than model predictions using eclipsing binary star DS And in the nearby open star the Gaia cluster distance. This points to issues with cluster NGC 752. We have measured high-precision conventional stellar models having masses slightly light curves in B, V, R and I filter bands, clearly show- above solar. We are grateful for funding from the ing a total secondary eclipse. From a spectral disen-

117 NSF under grant AAG1817217 to E.L.S., and NASA animations were published by SPACEWEATHER on under grant NNX15AW69G to R.D.M. the following dates: February 14 [5] and February 23 [6]. The pictures of the asteroid were captured 303.17 — High Precision Measurement of the with the following equipment: CGE PRO 1400 CE- Atlas Binary System Masses LESTRON (f/11 Schmidt-Cassegrain Telescope) and STL-1001 SBIG camera. Astrometry was carried out, 1 1 Peter Alexander Wysocki ; Eric L. Sandquist and we calculated the orbital elements. We obtained 1 Astronomy, San Diego State University (Darien, Illinois, United the following orbital parameters: eccentricity = States) 0.9920 ± 0.0148, = 160.405 ± 0.031 deg, longitude of the ascending node = 147.484 ± The Pleiades is a well-studied cluster with both white 0.011 deg, argument of perihelion = 358.06 ± 0.06 dwarfs and massive, young stars. We present new deg, perihelion distance = 1.287039 ± 0.000636 A.U, measurements of the radial velocities for both stars in mean motion = 0.00048 ± 0.00134 deg/d, absolute the interferometric binary Atlas in the Pleiades star magnitude = 12.2. The parameters were calculated cluster using the spectral disentangling method. Our based on 77 observations (Feb. 14-23) with mean large collection of archival spectral data allows for residual = 0.19 arcseconds. I also obtained the light more complete coverage of the radial velocity curve. curve of the body with our data. In particular, the extremes of the curve are much Acknowledgements: The author would like to better sampled. We use these measurements along thank to the University of Narino-Pasto-Colombia. with interferometric and lunar measure- [1] https://earthsky. ments of positions on the sky orbit to more precisely org/astronomy-essentials/ measure the orbital parameters. This in turn gives c-2018-y1-iwamoto-jan-feb-2019 a more precise measurement of the stellar masses. [2] https://www.space.com/ Along with the evolutionary state of the Atlas stars comet-iwamoto-visible-with-binoculars-february-2019. from photometry and the cooling time of the white html dwarfs, this greatly improves the initial mass deter- [3] https://scienceandtechblog. mination of the Pleiades white dwarfs for the initial- com/index.php/2019/02/07/ final mass relation. This will provide an independent comet-y1-iwamoto-tops-out-in-february/ determination of the age of the Pleiades that can be [4] https://sciencesprings. used to test other measures of the age, such as the wordpress.com/2019/02/01/ depletion boundary. from-earthsky-speedy-comet-approaching-earths-vicinity/ [5]http://spaceweathergallery.com/indiv_ 304 — iPoster Session: The Sun, upload.php?upload_id=151903 [6] http://spaceweathergallery.com/indiv_ Solar System & Public Policy upload.php?upload_id=152114

304.01 — The Comet Iwamoto (C/2018 Y1) 304.02 — Using Numerical Simulation to Consider the Observed Variations in the Behavior and Alberto Vodniza1 Appearance of Dark Spots on the Ice Giants 1 Physics, University of Narino Observatory (Pasto, Narino, Colombia) Raymond P. Le Beau1; Rebecca Loiacono1; Andrew Wagner1; Kevin Farmer1; Csaba J. Palotai2; Ramanaku- Comet Iwamoto was discovered by Masayuki mar Sankar2; Nathan Hadland2; Noah Nodolski2 Iwamoto on december 20, 2018. This comet has 1 Saint Louis University (Saint Louis, Missouri, United States) an orbital period of 1,371.3 years [1], and its next 2 Florida Institute of Techology (Melbourne, Florida, United States) passage around the sun will occur in the year 3390. The comet was closer to the earth on February 12 and The most recent observation of a dark spot on Nep- its distance to our planet was 45 million kilometers. tune (Simon et al., 2019) is the latest confirmation The perihelion occurred on February 7 [2]. The that these vortices are a not uncommon feature in comet reaches aphelion far beyond the Kuiper Belt the atmospheres of the Ice Giants. With observations in the world of Severe Trans-Neptunian Things [3]. of more than a half-dozen of these vortices since the This comet is traveling at a speed of 238,099 km/h, Voyager II encounters, we are now in a position to relative to Earth [4]. From our Observatory, lo- start categorizing the nature of these features and cated in Pasto-Colombia, I captured several pictures, try to determine what drives their different prop- videos and astrometry data during several days. The erties and behaviors. These behaviors can include

118 latitudinal and longitudinal drift, shape oscillations, too deep or insufficiently strong to develop visibly. and the formation of companion clouds. Simula- This could account for the cloud’s longevity as well tions of these dark spots with EPIC GCM (Dowling as the drift in latitude. Smith and Ulrich (1993) pos- et al., 2006) can capture all of these behaviors, pro- tulated that the gradient of the background absolute viding a diagnostic tool that can investigate the un- vorticity played a key role in vortex dynamics. To derlying physics of the observed phenomena. How- better understand this phenomenon, the EPIC GCM ever, these simulations have generally targeted a spe- (Dowling et al., 2006) was used to simulate the ex- cific feature such as the 1989 Great Dark Spot (GDS- istence of a dark spot in the observed region for the 89) or the Uranian Dark Spot (UDS), as opposed Berg. Multiple simulations featuring various back- to developing a consistent understanding that cap- ground vorticity gradients have been applied to in- tures the observed characteristics of all known dark vestigate the relationship between vorticity gradient spots. This more generalized work targets the effect and spot drift rate. This relationship will then be uti- of spot size, shape, and strength on its subsequent lized to determine an acceptable background vortic- evolution, examining for example its interaction with ity gradient field to simulate drift features compara- the zonal wind shears to generate drift or a lack of ble to the Berg’s observed drift rates. drift or the existence of orographic uplift-driven con- densation that may or may not generate companion 304.04 — Simulating Saturn’s A ring edge with a clouds. This systematic simulation of multiple vor- single chain of gravitationally-interacting particles tices and comparison of the results aims to reveal the 1 1 1 key physics that govern the observed differences be- Yuxi Lu ; Douglas P. Hamilton ; Thomas Rimlinger ; 2 tween the increasing number of recorded dark spots, Joseph M. Hahn 1 creating stronger links between the simulations and University of Maryland (College Park, Maryland, United States) 2 future observations. Space Science Institute (Austin, Texas, United States) The edge of the A ring, located 136,769 km from 304.03 — Numerical Simulations of Uranus’ Berg Saturn, has a 7-lobed pattern that appears and dis- Feature as a Vortex-Driven Cloud under Varying appears every 4 years as the nearby satellites Janus Background Vorticity Gradients and Epimetheus swap their orbital positions. While Kevin Farmer1; Raymond P. Le Beau1; Rebecca Janus is in the inner position, its 7:6 resonance from Loiacono1; Andrew Wagner1; Csaba J. Palotai2 Janus is located only ∼ 4 km inside the ring. This ex- cites the 7-lobed normal mode on the ring edge, and 1 Saint Louis University (St. Louis, Missouri, United States) the feature disappears as Janus moves from the inner 2 Florida Institute of Technology (Melbourne, Florida, United position to the outer. We wish to model this satellite- States) and have, accordingly, developed a new The Uranian Berg feature, first identified in the early code to do so. We modified the N-body code, hn- 2000’s, was a notable cloud feature in the southern body, to simulate narrow rings and ring edges us- hemisphere known for its visible similarity to an ice- ing a single chain of gravitationally-interacting parti- berg drifting off the Southern Polar Collar. This cles. We have tested our code on isolated resonances methane ice cloud remained in the region of 34° and can reproduce normal mode patterns includ- South until 2005 when it began a four-year equa- ing the 7-lobed feature in the A ring. However, the torward drift spanning roughly 20° (de Pater et al., outer portion of the real A ring is perturbed by sev- 2011). Similar behavior has been observed for some eral resonances. The four most important resonances large-scale geophysical vortices (dark spots) on the are The Lindblad Eccentric Resonances from Janus Ice Giants (Uranus and Neptune). Most notably, the and Epimetheus that affect the eccentricities and the original Great Dark Spot (GDS-89), observed by Voy- Corotation Eccentric resonances from each satellite ager II at Neptune, featured an equatorward drift of that primarily affect the semi-major axes. Moreover, its own over at least 10 degrees (Sromovsky et al., these four resonances move rapidly as the satellites 1993). The dark spots are so named for their darker swap orbital positions. We apply our new code to contrast to the surrounding atmosphere and for sev- simulate the A ring edge with both satellites present eral spots this contrast is further offset by bright oro- and we are able to study the global patterns on the graphic companion clouds that form above the vor- ring due to the action of multiple resonances. In tex. While the Berg did not feature any such dark this talk, we will describe how the outer parts of A contrast, the persistent bright clouds and drifting be- ring change over a Janus-Epimetheus orbital period havior suggests that the Berg may have had an un- in our simulations and we will compare our results derlying vortex beneath the observed cloud that was to observations.

119 305 — iPoster Session: Solar 305.02 — High-resolution Observations of Dynamics of Superpenumbral Hα Fibrils Physics Division (SPD), Session III Ju Jing1; Qin Li1; Chang Liu1; Jeongwoo Lee1; Yan Xu1; 305.01 — A CME-Producing Solar Eruption from Wenda Cao1; Haimin Wang1 the Interior of an Emerging Bipolar Active Region 1 New Jersey Institute of Technology (Newark, New Jersey, United States) Mitzi L. Adams1; Ronald L. Moore2; Navdeep Panesar1; David Falconer2 We present unprecedented high-resolution Hα ob- 1 NASA/MSFC (Huntsville, Alabama, United States) servations of a small solar pore in NOAA Active Re- 2 UAH/CSPAR (Huntsville, Alabama, United States) gion 12661, using the 1.6 m Goode Solar Telescope (GST) equipped with high-order adaptive optics at In a negative-polarity coronal hole, magnetic flux Big Bear Solar Observatory (BBSO). The observa- emergence, seen by the Solar Dynamics Observa- tions reveal copious fine-scale chromospheric super- tory’s (SDO) Helioseismic Magnetic Imager (HMI), penumbral fibrils (with a cross-sectional width of begins at approximately 19:00 UT on March 3, 2016. ∼0.15”) around the pore, along with associated tran- The emerged magnetic field produced sunspots, sit and intermittent flows with apparent speeds of5- which NOAA numbered 12514 two days later. The 20 km s−1. The wavelet analysis suggests that the emerging magnetic field is largely bipolar with the observed flows along fibrils are not likely a manifes- opposite-polarity fluxes spreading apart overall, but tation of oscillations, but rather collections of actual there is simultaneously some convergence and can- counterstreaming mass motions. The observed flow cellation of opposite-polarity flux at the polarity in- is interpreted as siphon flow. In addition, the three- version line (PIL) inside the emerging bipole. In dimensional potential field model indicates that the the first fifteen hours after emergence onset, three pore and the surrounding fibrils are enclosed by fan obvious eruptions occur, observed in the coronal field lines forming a separatrix dome configuration. EUV images from SDO’s Atmospheric Imaging As- We suggest that such a magnetically confined config- sembly (AIA). The first two erupt from separate uration may help to maintain the steadfastness of the segments of the external PIL between the emerg- superpenumbral fibril dynamics. ing positve-polarity flux and the extant surrounding negative-polarity flux, with the exploding magnetic 305.03 — Terminators: Predicting the end of field being prepared and triggered by flux cancella- sunspot cycle 24 and its impacts on space weather, tion at the external PIL. The emerging bipole shows weather and climate. obvious overall left-handed shear and/or twist in its magnetic field. The third and largest eruption Robert Leamon1; Scott W. McIntosh2 comes from inside the emerging bipole and blows it 1 Department of Astronomy, University of Maryland (College Park, open to produce a CME observed by SOHO/LASCO. Maryland, United States) That eruption is preceded by flux cancellation at 2 NCAR/ HAO (Boulder, Colorado, United States) the emerging bipole’s interior PIL, cancellation that plausibly builds a sheared and twisted flux rope Recent research has demonstrated the existence of above the interior PIL and finally triggers the blow- a new type of solar “event.” Unlike the signature out eruption of the flux rope via photospheric- events in the corona, flares and Coronal Mass Ejec- convection-driven slow tether-cutting reconnection tions, this event, the Terminator, takes place in the so- of the legs of the sheared core field, low above the lar interior (at the Sun’s equator), signalling the end interior PIL, as proposed by van Ballegooijen and of a magnetic activity cycle and the start of a sunspot Martens (1989, ApJ, 343, 971) and Moore and Roume- cycle at mid latitudes – all at the same time. Observa- liotis (1992, in Eruptive Solar Flares, ed. Z. Svestka, tions indicate that the hand-over between the termi- B.V. Jackson, and M.E. Machado [Berlin:Springer], nation of the magnetic activity cycle and the bloom- 69). The production of this eruption is a (perhaps ing of the next sunspot cycle could be very short, pos- rare) counterexample to solar eruptions that result sibly much less than a solar rotation. from external collisional shearing between oppo- Here we demonstrate the impact of these termi- site polarities from two distinct emerging and/or nators on the Sun’s radiative output and particulate emerged bipoles (Chintzoglou et al., 2019, ApJ, shielding of our atmosphere through the dramati- 871:67). cally rapid reconfiguration of solar magnetism. Us- This work was supported by NASA, the NASA Postdoc- ing direct observation and proxies of solar activity toral Program (NPP), and NSF.

120 going back six decades we can, with high statisti- I present initial results from a systematic look at pos- cal significance, demonstrate an apparent correlation sible indicators of active region emergence precur- between the solar cycle terminations and the largest sors using acoustic power mapping and time dis- swings of Earth’s oceanic indices – a previously over- tance travel time anomalies. Using HMI observa- looked correspondence. tions I have analyzed a set of active regions that have We then use a standard method in signal process- emerged at low latitudes and close to the central ing, the Hilbert transform, to investigate the pres- meridian. Since these regions emerged close to disk ence, and identify the signature, of terminators in center, they could be tracked for days before and af- solar magnetic and radiative proxies. Using many ter their emergence. Data cubes of tracked surface decades of such data we can achieve higher fidelity images of various lengths were analyzed using both on terminator timing than previous estimates have intensity and velocity observations. While each ac- allowed. tive region exhibits particular properties, this sys- The distinct signature presents a unique opportu- tematic approach allowed me to look at a few sta- nity to project when the next terminator will occur, tistical properties that will be summarized. Namely April 2020 (± two months) and sunspot cycle 25 will the trade-off between precision and resolution, both commence its growth phase. Further, April 2020 im- temporal and spatial resolution, and the correlation plies cycle 24 will only be 9.25 years long; we offer between various metric of surface activity and its im- an explanation as to why cycle 24 is short (or rather, pact of the measured acoustic signal, whether seen in why cycle 23 and its “unusual solar minimum” was power map (filtered or not) or travel time anomalies so long). derived from a time-distance analysis (also using a Finally, should a major ENSO swing follow next few different filtering). year, our challenge becomes: when does correlation become causation and how does the process work? 306 — iPoster Session: 305.04 — Coronal Magnetic Field Topologies of Supernovae, AGN & Galaxies Solar Active Regions 306.01 — Core-Collapse Supernova Light Curves Marc L. DeRosa1; Graham Barnes2 1 Lockheed Martin Solar and Astrophysics Laboratory (Palo Alto, Morgan Taylor2,1; Wesley P. Even2; Ryan Wollaeger2 California, United States) 1 Applied Math, Southern Utah University (Taylorsville, Utah, 2 NorthWest Research Associates (Boulder, Colorado, United States) United States) 2 Los Alamos National Laboratory (Los Alamos, New Mexico, The magnetic field overlying the coronae of solar ac- United States) tive regions displays many complex configurations. In this work, we show renderings of the impor- Core-collapse supernovae are challenging phenom- tant topological surfaces corresponding to potential ena to simulate realistically from first principles. fields above solar active regions. Common geome- Light curves from such events provide an abundant tries are identified, such as nested domains of con- source of data, helping to constrain theoretical mod- nectivity, and the presence of narrow channels of els. They can be used indirectly to determine the open flux having high expansion factors. Addition- possible kinetic energies, masses, and compositions ally, a sequence of magnetic field topologies is used of the explosion outflows. In this project, we takea to demonstrate null-point creation and annihilation. suite of core-collapse supernovae models with var- Due to the presence of electric currents, the real coro- ious explosion energies, and post process to gener- nal magnetic field topology is expected to be even ate light curves. The progenitor masses used are 15, more complex than that found in these potential 20, and 25 M⊙. We use the radiative transfer code fields. SuperNu to construct the light curve data. We then compare our results to observed core-collapse light 305.05 — On the search of active region emergence curves to identify realistic explosion models from the precursors using acoustic power maps and travel suite. time anomalies derived from time-distance analysis of HMI observations 306.02 — Magnetohydrodynamic Jet Simulations for Radio-loud AGN Sylvain G. Korzennik1 1 Center for Astrophysics | Harvard & Smithsonian (Cambridge, Xuanyi Zhao1; Nicholas Tusay1; Terance Schuh1; Massachusetts, United States) Nicholas Juliano1; Paul J. Wiita1

121 1 Physics, The College of New Jersey (Ewing Township, New Jersey, Of galaxies investigated, 50% reveal evidence of dust United States) heating surrounding super-massive black holes, but lack an X-ray detection. We X-ray stack these galaxies We present three-dimensional magnetohydrody- to obtain hard and soft fluxes, allowing us to measure namic jet simulations relevant to extragalactic ra- the energetics of these AGN. Stacking allows us to dio galaxies and quasars. We utilized an updated determine obscuration and X-ray luminosities to cal- Athena++ code to incorporate magnetic fields into culate accretion rates. Results show that these galax- previously computed high-resolution hydrodynam- ies are more extended and have higher SFRs than ics simulations. In addition to identifying the turbu- their unobscured counterparts. This work demon- lence and shock structures within the jet and cocoon, strates that there is a higher population of obscured we explored the change of jet behavior resulting from AGN than previously thought. Our results fit in with by the effects of dynamically important magnetic the paradigm where obscured AGN directly proceed fields. We examined the different jet propagations an unobscured phase, this unobscured phase is fol- for a variety of jet velocities, jet-to-ambient gas den- lowed by quenching of star formation. sity ratios and different magnetic field strengths and morphologies within the jet stream and in the sur- 306.04 — A New Population of Cold Quasars rounding medium. These comparisons of the behav- iors of the MHD jets allows us to better categorize Brandon Coleman1; Allison Kirkpatrick1; Jordan each jet’s outcome as either a Fanaroff-Riley I (jet- Johnson1; C. Megan Urry2; David B. Sanders3; Eilat dominated) or FR II (radio lobe-dominated) radio- Glikman4 loud active galactic nucleus. We also compared the 1 Physics and Astronomy, University of Kansas (Lawrence, Kansas, results produced from simulations with different United States) resolutions and noted increases in turbulence and jet 2 Yale University (New Haven, Connecticut, United States) asymmetry at higher resolution. 3 University of Hawaii (Honolulu, Hawaii, United States) 4 Middlebury College (Middlebury, Vermont, United States) 306.03 — Where do Obscured AGN fit in the AGNs are the most luminous objects in the universe, Galactic Timeline? and the most massive ones are usually created by the Cassandra Hatcher1; Dr. Allision Kirkpatrick1; merger of two gas-rich disk galaxies. This gas fuels Francesca Civano2; Francesca Fornasini2 an AGN through an accretion disk that emits at opti- 1 University of Kansas (Lawrence, Kansas, United States) cal/ultraviolet wavelengths. This accretion disk can 2 Smithsonian Astrophysical Observatory (Cambridge, Mas- be obscured by a dusty torus that emits mostly in the sachusetts, United States) IR waveband. Towards the center of the AGN, an energetic corona emits in the X-Ray waveband. We X-ray bright active galactic nuclei (AGN) are pre- have identified >1800 X-ray luminous AGN ina16 dicted to follow an extended stage of obscured black deg2 region of the Stripe82 field surveyed by XMM- hole growth, after which they produce most of their Newton and Herschel. Given the detection limits of feedback. In support of this picture we examine the Herschel, only 10% of our AGN have both an X-ray most heavily obscured AGN in three different fields detection and an IR detection, providing unique in- and compare their host galaxies with X-ray bright sight into the fraction of luminous AGN surrounded 9.5 AGN. We examine galaxies (M > 10 M⊙ for the by an abundance of cold dust. We coin these IR presence of AGN at redshifts z = 0.5 - 3 in the COS- bright, type-1 AGN “cold quasars”. We demonstrate MOS, EGS, and GOODS-S fields. We select AGN that many of these cold quasars are in the canoni- in the infrared and correlate different infrared selec- cal coalescence phase by examining SDSS imaging. tion techniques to assess their reliability. This in- However, just as many appear to be isolated point cludes probing the full shape of the IR spectral en- sources, challenging the merger scenario. We com- ergy distribution by combining Herschel and Spitzer pare the IR luminosity and X-ray luminosity with colors, 250/24 μm and 8/3.6 μm. 250/24 traces the less X-ray luminous AGN from z=1-2 (from COSMOS ratio of the far-IR to mid-IR emission; lower ratios and GOODS-S) and find cold quasars to have pro- correlate with AGN heating. 8/3.6 traces the stellar portionally more X-ray emission at a given infrared bump; in this regime AGN radiation will outshine luminosity. This is likely due to the IR emission aris- the stellar bump. These colors were correlated with ing from the host galaxy, while the X-ray emission full SED fitting for a few sources to verify the accu- comes from the AGN component. We also compare racy of this method. These IR colors allow us to se- the amount of dust mass in these cold quasars with lect AGN within strongly star forming host galaxies. the dust mass of star formation galaxies at the same

122 redshifts and find it to be comparable. This then sup- galaxy evolution - the aging, evolution, merging his- ports the picture where the quasar component is just tory of galaxies. This project involves determining beginning to become luminous, but has not blown the separation of the peak of X-ray emission of the out any of the host galaxy gas and dust. , and the location of the BCG. We do this to characterize the system as being disturbed or 306.05 — Accretion History of AGN: Measuring undisturbed. We have found that ∼17% of the 23 sys- Black Hole Masses in Cold Quasars tems we observed have large separations, and thus may have undergone a recent merging event. Pre- 1 1 Michael Estrada ; Allison Kirkpatrick ; C. Megan liminary results on the age, metallicity and kinemat- 2 3 4 Urry ; David B. Sanders ; T. Jane Turner ics of the BCGs with large and small systems will be 1 Physics, University of Kansas (Lawrence, Kansas, United States) compared and presented. 2 Yale University (New Haven, Connecticut, United States) 3 University of Hawaii (Honolulu, Hawaii, United States) 4 306.07 — The distribution of ages, metallicities UMBC (Baltimore, Maryland, United States) and dynamics of stellar populations in 23 BCGs using the SparsePak IFU In the SDSS Stripe 82X field, the Accretion History of AGN (AHA) collaboration has assembled a multi- Priscilla Elise Holguin West1; Louise O. V. Edwards1 wavelength dataset of thousands of X-ray luminous 1 California Polytechnic State University (San Luis Obispo, Califor- AGN. From this parent population, we select quasars nia, United States) in host galaxies at z<1 which are also strongly star forming, as measured in the far-IR. This yields 59 Local Brightest Cluster Galaxies (BCGs) are the most quasars which have far-IR star formation rates, X-ray massive galaxies in the local universe and have had luminosities, spectroscopic redshifts, and SDSS opti- the full age of the universe to build. We present the cal spectra covering the broad emission line region. radial profile of ages, metallicities, and dynamics of Eight of the 59 galaxies exhibit broadening of the 23 BCGs observed using the SparsePak instrument H-α emission, which we use to measure black hole on WIYN by running the STARLIGHT stellar popu- mass. The broadening behavior of the line is caused lation synthesis models. Preliminary results of the by the motion of the gas under the gravitational in- stellar populations for different regions of the BCG, fluence of the black hole. We fit Gaussian models such as its core and outskirts, the intracluster light to the broad emission line and to the narrow H-α (ICL), and close companions of the BCG, are pre- peak in order to separate these two physically dis- sented. The BCG core is found to host an older, tinct components. We use the flux and FWHM of the more metal-rich population of stars than those found H-α line to estimate the black hole mass. We com- within the ICL. Analysis of the velocity dispersion bine these masses with the bolometric luminosities as a function of the distance from the galactic center (calculated from the X-ray luminosities) to determine yields a rising or flat profile for ∼70 percent of our each quasar’s Eddington ratio, a measure of how effi- X-ray selected sample. cient the black hole is at accreting mass. We compare the Eddington ratios for our quasars with published 306.08 — Antila2: the dark dwarf galaxy that literature values to determine if quasars that are still crashed into the Milky Way forming stars (at rates >50 Msun/yr) show enhanced 1 or decreased activity with respect to other samples. Sukanya Chakrabarti 1 RIT (Rochester, New York, United States) 306.06 — The offset of Brightest Cluster Galaxies Some time ago, we analyzed perturbations in the from their parent cluster core outer gas disk of the Milky Way (Chakrabarti & Blitz Matthew Aaron Salinas1; Louise O. V. Edwards1 2009) and predicted how massive and how close a 1 Physics, California Polytechnic State University, San Luis Obispo dark-matter dominated dwarf galaxy would have to (Dinuba, California, United States) get to produce the disturbances in the outer HI disk of our Galaxy. The prediction was that a massive A Brightest Cluster Galaxies (BCG) is the bright- dwarf galaxy (about one-hundredth the mass of our est galaxy in a cluster of hundreds to thousands of Galaxy) with a close pericenter approach (about 7 - galaxies. These monsters are some of the biggest, 10 kpc) was needed to explain the large perturbations brightest, and most massive galaxies in the universe. at the edge of our Galaxy. We also predicted that it Characterizing a BCG can help discover more about would currently be at a distance of ∼100 kpc from the Galactic center. Many of the observed parameters of

123 the Antlia2 dwarf galaxy are similar to our prediction the observations and simulations, we benchmark di- from ten years ago. Using the observed Gaia proper agnostics of the magnetic field strengths and thermal motions of the Antlia2 dwarf galaxy, we have deter- properties of the solar corona on global scales. We mined its orbital distributions, and its effect on the discuss the future prospects of using such extreme Galactic disk. The low pericenters of the orbital dis- EUV waves as probes for global coronal seismology, tribution are sufficent to explain the observed distur- an area yet to be fully exploited. bances in the outer HI disk of the Milky Way. Such an interaction, i.e., very similar to our prediction in 307.02 — Transient dynamics and energy transfer Chakrabarti & Blitz (2009), also reproduces the ve- from the photosphere to the low corona: initial locity sub-structures seen in the Gaia DR-2 data. We results from a coordinated ALMA, DST, Hinode, argue therefore that the giant, yet faint, dwarf galaxy IRIS, and SDO observation campaign Antlia2 is the very likely the culprit that produced 1 2 3 the ripples in the outskits of the Milky Way. Adam Kobelski ; Lucas A. Tarr ; Sarah A. Jaeggli ; Sab- rina Savage4 1 Department of Physics and Astronomy, West Virginia University 307 — iPoster Plus IX: (SPD) (Morgantown, West Virginia, United States) 2 Eruptions, George Mason University (Fairfax, Virginia, United States) 3 National Solar Observatory (Maui, Hawaii, United States) Photosphere/Chromosphere, 4 NASA MSFC (Huntsville, Alabama, United States)

Helioseismology and Solar We present initial results from a coordinated obser- Interior vation campaign to study transient dynamics and en- ergy transfer in the low solar atmosphere. The ob- 307.01 — The Global EUV Wave Associated with servations ran from approximately 2017-03-21 from the SOL2017-09-10 X8.2 Flare: SDO/AIA 13UT to 19UT, and include data from Hinode, IRIS, Observations and Data-constrained MHD DST, and ALMA. The target, a small, magnetically Simulations bipolar active area associated with a coronal bright point, was chosen for showing reasonable dynamics Wei Liu1; Meng Jin2; Leon Ofman3; Marc L. DeRosa2 in the chromosphere (as dictated by AIA 304 data 1 Stanford-Lockheed Institute for Space Research (Palo Alto, Califor- from the day prior), and being near disk center to nia, United States) better facilitate magnetic field measurement. The 2 lockheed martin solar and astrophysics laboratory (Palo Alto, campaign was designed to capture the dynamics of California, United States) the target with as rapid a timescale as possible for 3 The Catholic University of America (Washington, District of each instrument. Photospheric dynamics are avail- Columbia, United States) able from broadband IBIS data and the HMI. New to this dataset, the chromospheric dynamics were ob- While large-scale extreme ultraviolet (EUV) waves served in radio frequencies using ALMA (Band 3: 92- associated with coronal mass ejections (CMEs) and 108GHz) at a 2s cadence. Additional chromospheric solar flares are common, the EUV wave triggered by data are spectral H-α from the IBIS instrument at the the X8 flare-CME eruption on 2017 September 10 was DST, spectropolarimetic HeI 10830 from the FIRS in- an extreme. This was, to the best of our knowledge, strument at the DST, and the medium linelist from the first detection of an EUV wave traversing the full- IRIS; coronal data includes imaging from XRT and Sun corona over the entire visible disk and off-limb spectral data from EIS. In this first set of results, we circumference, manifesting a truly global nature. In discuss the frequency of transient brightenings ob- addition to commonly observed reflections, it had served in each set of imaging data and how the spa- strong transmissions in and out of both polar coronal tial distribution relates across each data channel and holes, at elevated wave speeds of >2000 km/s within to the regions magnetic topology. them. With an exceptionally large wave amplitude, it produced significant compressional heating to lo- 307.03 — Detection of Dynamo Waves in the Solar cal coronal plasma. We present detailed analysis Convection Zone by Helioseismology of SDO/AIA observations, global magnetic field ex- trapolations with the potential-field source surface Alexander G. Kosovichev1; Valery Pipin2 (PFSS) model, and data-constrained MHD simula- 1 New Jersey Institute of Technology (Newark, New Jersey, United tions of this event using the University of Michigan States) Alfven Wave Solar Model (AWSoM). By comparing 2 Institute of Solar-Terrestrial Physics (Irkutsk, Russian Federation)

124 Analysis of helioseismology data obtained in 1996- of such perturbations on emergent intensity and ve- 2019 for two solar cycles from two space missions, locity and estimate their impact on helioseismic ob- Solar and Heliospheric Observatory (SoHo) and So- servables. lar Dynamics Observatory (SDO), reveals that latitu- dinal variations of solar rotation (’torsional oscilla- 307.06 — Listening to the Sun: the Sonification of tions’) are associated with hydromagnetic dynamo Solar Harmonics Project waves initiated in the solar tachocline and travelling 3 1 2 in radius and latitude towards the surface during the Timothy P. Larson ; Seth Shafer ; Elaine diFalco 1 solar cycles. On the surface, the waves form two School of Music, University of Nebraska at Omaha (Omaha, Ne- branches of zonal deceleration migrating towards braska, United States) 2 the poles and equator, and coinciding with the large- Department of Media Arts, University of North Texas (Denton, scale magnetic field patterns observed in synoptic Texas, United States) 3 magnetograms. The results explain the phenomenon Moberly Area Community College (Columbia, Missouri, United of ’extended solar cycle’, and provide first obser- States) vational evidence for magnetic dynamo waves pre- Helioseismology has enjoyed far-reaching success dicted by the Parker’s theory of solar activity cycles. over the last few decades. Not only has it enabled We compare the observational results with dynamic physical inferences of unprecedented precision, but models of the solar dynamo, and discuss driving when one learns for the first time that the Sun isa mechanisms of the torsional oscillations. resonant cavity for low frequency sound waves, the reaction is almost always one of wonder and awe. 307.04 — (withdrawn) The question naturally arises: ”What does it sound This abstract was withdrawn. like?”. Unfortunately, until now, helioseismologists have rarely been able to give a satisfying response. Although we spend our days studying sound waves, 307.05 — Modeling observables for local we never listen to our data. The purpose of the Soni- helioseismology. fication of Solar Harmonics (SoSH) Project is tomake Nadiia Kostogryz1; Damien Fournier1; Laurent Gizon1 such listening accessible to scientists and nonscien- 1 Max Planck Institute for Solar System Research (Goettingen, tists alike. Germany) We have developed software that closely mimics global-mode helioseismic data processing and also Local helioseismology provides different techniques uses the results thereof. The SoSH Tool, as we have to study flows in the solar interior. However, all called it, filters real solar data and transposes itupto of them suffer from systematic errors, which occur the range of human hearing, all the while preserving because of the nontrivial relationship between wave the frequency relationships between the modes. In displacement and helioseismic observables, such as other words we retain the musical intervals between intensity and Doppler velocity. In this study, we solar harmonics, thus enabling one to use the Sun solve the radiative transfer equation in a perturbed like a musical instrument. solar atmosphere including flows caused by acous- Creative applications are not the only use of the tic oscillations. The adiabatic oscillations for nor- SoSH Tool. Sonification has been used extensively in mal modes of low and high degree are computed us- the study of geoseismology as well as other types of ing the ADIPLS code that solves an eigenvalue prob- solar data. Thus, we have reason to suspect that the lem in a standard solar model assuming spherically auditory modality may also have advantages over symmetric background quantities. The wave dis- purely visual display when it comes to helioseismol- placement causes perturbations in atmospheric ther- ogy. Further, we already know that solar rotation is modynamical quantities that, in turn, perturb opac- easily heard in the sonified data, as well as the so- ity and emergent intensity. These perturbations de- called small frequency separation, which is sensitive pend on the center to the limb distance. In addition, to conditions in the solar core. If we sacrifice the mu- the oscillations modify the shape of the solar sur- sical intervals between tones, we can also hear the so- face and thus the direction of the normal to the sur- lar cycle. face. For low-degree modes this geometrical effect Several extensions and new applications of the is negligible, however, this effect matters for high- SoSH Tool are underway. We have written a python degree modes with a large horizontal component of module to create graphical representations of the wave displacement. We investigate the contribution modes we sonify. This will eventually lead to full- dome planetarium presentations of the interior of the

125 Sun. The SoSH Tool is able to combine solar harmon- universe under several circumstances. Apart from ics in a variety of ways, and this will enable the com- that we determine if trajectories in the proximity of position of a solar concerto. As we sonify and make a critical point are attracted or repelled by the point public larger volumes of sonified data, we hope to itself or, in other words, to study the stability prop- not only spread knowledge of helioseismology, but erties of the critical point and acceleration phase of perhaps to also reap new scientific insights. the universe which could then be analyzed with ob- servational data.

308 — Cosmology & Related 308.03 — ΛCDM is in tension with Pantheon data Topics at 4.3σ in ωm Maurice H. Van Putten1 308.01 — The Limitations of Redundant 1 Physics and Astronomy, Sejong University (Seoul, Seoul, Korea Calibration for Radio Interferometry and 21 cm (the Republic of)) Cosmology Jonathan Pober1 Surveys of the Local Universe show a Hubble ex- 1 Brown University (Providence, Rhode Island, United States) pansion significantly greater than ΛCDM estimates from the Cosmic Microwave Background by Planck. The idea of redundant calibration has a long history We here report on a 4.3σ tension in ωm = Ω푚,0in in radio interferometry, but has drawn renewed at- Pantheon data, independent of Planck, observed in tention over the last several years for its potential a novel probe over running intervals [0,zmax] (0 < to mitigate systematics in 21 cm cosmology exper- z푚푎푥< 2.26). This tension reduces to 2.5σ in late time iments. In this talk, I will show results from both quantum cosmology, wherein de Sitter space is un- simulations and the analysis of real data that demon- stable by dark energy induced by the cosmological strate the limitations inherent to redundant calibra- horizon with implied deviations from ΛCDM at the tion. In particular, many of the frequency-dependent present epoch. calibration errors that plague 21 cm cosmology can- not be mitigated by redundant calibration. Without 308.04 — A standard ruler at cosmic dawn alternative methods, ”traditional” sky-based calibra- 1 tion schemes remain an essential part of a 21 cm cos- Julian B. Munoz 1 mology analysis pipeline – and the challenges associ- Physics, Harvard University (Cambridge, Massachusetts, United ated with sky-based calibration must continue to be States) addressed. Dark matter and baryons posses supersonic rela- tive velocities after recombination, as only the lat- 308.02 — Stability analysis using dynamical ter suffers baryon acoustic oscillations (BAOs). These systems in modified gravity velocities—imprinted with the acoustic scale in their Parth Mukeshbhai Shah1 genesis—impede the formation of the first stars dur- 1 Mathematics, BITS Pilani, KK Birla Goa Campus (Goa, Goa, ing the cosmic dawn (z=20), modulating the ex- India) pected 21-cm signal from this era, and inducing new velocity-induced acoustic oscillations (VAOs) in the Modified gravity theories have received increased at- 21-cm power spectrum. I will explain how to use tention lately to understand the late time acceleration these VAOs as a standard ruler at cosmic dawn, for of the universe. This viewpoint does not need unde- which we take advantage of the immunity of VAOs tected candidates like dark energy and dark matter to the unknown astrophysics of the first stars. I will at fundamental level and it takes into account only show that the upcoming HERA interferometer will the “observed” quantities. Among numerous exten- be able to measure the Hubble expansion rate H(z) sion to Einstein’s theory of gravity, theories which at z = 17 − 21 to percent-level precision using VAOs. include higher order curvature invariant, and specif- ically the class of f(R) theories, have received sev- 308.05 — An interactionless Ising model for galaxy eral acknowledgments. In our current work we try bias to understand the late time acceleration of the uni- 1 verse by modifying the geometry of the space and Andrew Repp 1 using dynamical system analysis. The use of this Astronomy, University of Hawaii, Institute for Astronomy (Hon- technique allows to understand the behavior of the olulu, Hawaii, United States)

126 Galaxy surveys, such as the upcoming Euclid and Sitter spacetime geometry. Hence, the two models WFIRST missions, represent an important observa- might be distinguished either by grand-scale obser- tional constraint on cosmology. However, the fact vations of the “jerk” of cosmic expansion, or by the that galaxies are biased tracers of the underlying quantum behavior of elementary-particle fields, or dark matter complicates the extraction of informa- both. tion from these surveys. In addition, the focus of current bias models is the high-density regions of 308.08 — Ultra-High-Energy Cosmic Ray the Universe, but low-density regions carry signifi- Acceleration by Hyper-Resistive Diffusion from cant information relevant to dark energy and alterna- Magnetic Tower Jets tive gravitational theories. Thus it is necessary for a 1,2 2 3 galaxy bias model to be accurate at both high and low Richard Anantua ; T. Kenneth Fowler ; Hui Li 1 densities. We here present such a model (inspired by Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- the Ising model of ferromagnetism), and we demon- sachusetts, United States) 2 strate its good fit to both simulations and observa- UC Berkeley (Berkeley, California, United States) 3 tional data. The quality of the fit indicates that, toa Los Alamos National Laboratory (Los Alamos, New Mexico, first approximation, galaxy formation is a local pro- United States) cess determined by initial conditions. Accretion disk dynamo currents are shown to power relativistic jets in a two-quasi-steady-state model 308.06 — LISA for Cosmologists with hyper-resistive diffusion, in which a conical 1 Robert Caldwell jet with Er = B휑 can be decelerated by the ambient 1 Physics & Astronomy, Dartmouth College (Hanover, New Hamp- medium to form a magnetic tower jet with j x B = 0. shire, United States) In the central column of the jet, the electron current is suppressed by a two-stream instability, and ions We survey the ability of the Laser Interferometer are preferentially accelerated over synchrotron radi- Space Antenna to address questions of cosmology. ating electrons. In the jet-lobe boundary, or nose, We present new results on Standard Siren tests of ions are further accelerated via drift cyclotron loss the cosmic expansion history at high redshift, and cone (DCLC) instability to the highest energies ob- probes of the early Universe in the form of a stochas- served for cosmic rays (>0.1 ZeV). Other predictions tic gravitational wave background. of this model include: jet maximum length (L = 1024 cm), width (R = 0.1L) and synchrotron luminosity 43 308.07 — Tachyon-Dominated Cosmology (P = 1.4x10 M8 erg/s) and cosmic ray spectrum (∼ E−3) and intensity (1/km2 century) all concordant 1 Ian H. Redmount with observations from distant galaxies. 1 Saint Louis University (St. Louis, Missouri, United States) 308.09 — Confirmation of Planet-Scale Although tachyons—faster-than-light particles— Astronomical Dark Matter in Extragalactic are usually regarded as fanciful speculation, it is Systems possible to construct a straightforward Einsteinian dynamics and thermodynamics governing such Saloni Bhatiani1; Xinyu Dai1; Eduardo Guerras1 particles. The mass/energy density of a gas of 1 Physics and Astronomy, University of Oklahoma (Norman, Okla- “dark” tachyons is such that an open—spatially homa, United States) hyperbolic—Friedmann-Robertson-Walker space- time dominated by such a gas can undergo the Quasar microlensing serves as a unique probe of same large-scale evolution as the standard dark- discrete objects within galactic-scale lenses such as energy/cold-dark-matter model: expansion from galaxies and galaxy clusters. Recent advancement an initial singularity at a rate which decelerates to of the technique shows that it can constrain planet- a minimum, passes through a “cosmic jerk,” and scale objects by studying their induced microlensing subsequently accelerates. Features of such a model signatures, the energy shift of emission lines origi- can be calculated and compared with observations. nated at the vicinity of the black hole of background Of particular interest is the fact that the tachyon- quasars, beyond our native galaxy. We employ this dominated model asymptotically approaches a technique to exert effective constraints on the sub- constant expansion rate and flat spacetime ge- stellar mass distribution within two additional ex- ometry, in contrast to the standard model, which ternal lens systems, Q J0158−4325 (zl = 0.317) and expands exponentially in time and approaches de

127 SDSS J1004+4112 (zl = 0.68) using Chandra observa- cannot reproduce experimental results reliably, es- tions of the two gravitationally-lensed quasars. The pecially in the C-H stretching region (∼3.3 μm) and frequently observed variations of the emission line combination band region (∼5 μm). In order to peak energy can be explained as microlensing of account for these deficiencies, anharmonic correc- the FeKα emission region induced by planet-sized tions need to be incorporated. Specifically, a sec- microlenses. To corroborate this, we perform mi- ond order vibrational perturbation theory approach crolensing simulations to determine the probability is used in this work, which also takes into account the of a caustic transiting the source region and com- large number of vibrational resonances predicted for pare this with the observed line shift rates. Our PAHs. analysis yields constraints on the sub-stellar popula- Additionally, the process in which PAHs absorb tion, with masses ranging from Moon (10−8 M⊙) to and emit energy in interstellar space is complex. Jupiter (10−3 M⊙) sized bodies, within these galaxy- PAHs are electronically excited by ultra-violet (UV) scale structures. Our results suggest that planet- photons from a nearby star, then through an emis- scale astronomical dark matter is universal in exter- sionless intraconversion process they drop to their nal galaxies, and we surmise these objects to be ei- electron ground state, and in doing so transfer the ther free-floating planets or primordial black holes. energy into their many vibrational modes. Then We present the first ever constraints on the sub-stellar through a slow emission process, they emit this en- mass distribution in the intra-cluster light of a galaxy ergy in the IR. This so-called cascade spectra results cluster. in an ever–changing internal vibrational energy (i.e., temperature) as the PAHs cool. Therefore, accurate calculations of anharmonic temperature effects are 309 — Laboratory Astrophysics also required for every internal temperature visited Division Meeting (LAD): Bridging during the cascade process. In this work we present a fully anharmonic IR cascade model (which includes Laboratory & Astrophysics: recalculating resonances at each internal tempera- Molecules and Spitzer III ture), reproducing the actual type of PAH spectra which astronomers directly observe. 309.01 — LAD Dissertation Prize: Producing accurate theoretical anharmonic infrared cascade 309.02 — Exploring Dust Composition in Debris spectra of PAHs Disks Cameron J. Mackie1; Alessandra Candian2; Timothy J. Alycia J. Weinberger1; Jessica A. Arnold1; George D. Lee3; Alexander Tielens2 Cody1; Gorden Videen2; Evgenij S. Zubko3 1 1 Lawrence Berkeley National Laboratory (Walnut Creek, Califor- Carnegie Inst. Of Washington (Washington, District of Columbia, nia, United States) United States) 2 2 Leiden Observatory (Leiden, Netherlands) Space Science Institute (Boulder, Colorado, United States) 3 3 NASA Ames Research Center (Mountain View, California, United Far Eastern Federal University (Vladivostok, Russian Federation) States) Planetesimals left over from planet formation collide The infrared (IR) signatures of polycyclic aromatic to generate dust around mature stars, observed as hydrocarbons (PAHs) have been observed in numer- debris disks. The dust composition provides evi- ous astronomical objects: from young stellar objects, dence for the material out of which planets form. to planetary nebulae, to the emissions of galaxies We are accumulating a wealth of as a whole. Not only are these PAHs found in var- imaging and spectroscopy: Hubble Space Tele- ied environments, their spectral features are like- scope and ground-based adaptive optics imagers for wise varied; indicating changes in properties such as for scattered light at visible to near-infrared wave- size, structure, charge, temperature, hydrogenation, lengths, Spitzer Space Telescope for mid-infrared nitrogen substitutions, etc. Interpretation of these spectrosocpy and Spitzer and Herschel for mid to spectral features and their variations relies heavily far-infrared spectral distributions, and ALMA for on theoretical calculations. Until now, the majority submm emission from large grains observed at high of these theoretical IR spectra make use of scaled har- angular resolution. The combination of data can be monic frequencies for band positions, and the dou- sensitive to important and astrobiologically relevant ble harmonic approximation for intensities. How- planetary constituents such as silicates (rock), water ever, low-temperature high-resolution gas-phase ex- ice and carbonaceous compounds as well as grain periments have shown that the harmonic treatment size distributions related to the dynamics of the disk.

128 However, interpretation of scattered light and tory studies are briefly discussed focusing on these emission measurements simultaneously to provide rates. unique constraints on the dust properties is diffi- cult. The solution likely sits with new grain measure- 309.04 — Combined Experimental and Theoretical ments and calculations. Study of Atomic Deuterium Reacting with + As well as reviewing the field, I will show our H3 Isotopologues new discrete dipole calculations made with the goals 1 1 of creating grains that can both fit the scattered Kyle Patrick Bowen ; Pierre-Michel Hillenbrand ; 3 2 1 and thermal light, grains that include all major con- Jacques Lievin ; Xavier Urbain ; Daniel Wolf Savin 1 situents in a more physical way than mixing the- Columbia Astrophysics Laboratory (New York, New York, United ory, and grains that properly predict the measured States) 2 phase functions of real particles and of debris disks. Université catholique de Louvain (Louvain-la-Neuve, Belgium) 3 We are guided by interstellar and solar system dust Université Libre de Bruxelles (Brussels, Belgium)

analogs. Currently, we have a significant set of calcu- + The partially deuterated isotopologues of H3 lations for irregularly shaped particles both of homo- + + geneous composition and of mixtures of astrosilicate (H2D and D2H ) play a prominent role in prestellar with ice and carbonaceous components. We have in- cores. At the typical densities and temperatures of prestellar cores, most species freeze onto dust grains. vestigated how our realistic morphologies affect the + radiation pressure blowout sizes expected in debris However, H3 and its isotopologues remain in the disks and find a strong dependence. gas-phase and become the dominant positive charge We are also taking laboratory spectra and comput- carriers. This affects the dynamics of core collapse ing indices of refraction to extend the range of ma- through the coupling of the gas to any ambient mag- netic fields. For this reason, knowledge of the total terial available for debris disk modeling. Our mea- + abundance of H3 and its isotopologues is critical surements of an analog to meteoritic insoluble or- + for modelling a core’s evolution. The symmetric H3 ganic material show similarities to previously mea- + sured organics and are quite different from amor- and D3 do not have dipole moments, and therefore phous carbon or . lack pure rotational spectra, rendering them unob- servable at prestellar core temperatures. Determin- ing the abundance of H D+ and D H+, which have 309.03 — Dicarbon formation in collisions of two 2 2 pure rotational spectra that can be excited at prestel- carbon atoms + lar core temperatures, allows for the total H3 abun- James F. Babb1; Ryan T. Smyth1,2; Brendan dance to be inferred, provided the deuterating re- 1,2 + McLaughlin actions of H3 are well understood. Deuteration of 1 + + + + + Center for Astrophysics | Harvard & Smithsonian (Cambridge, H3 ,H2D , and D2H forming H2D ,D2H , and + Massachusetts, United States) D3 , respectively, can occur either in reactions with 2 Queen’s University Belfast (Belfast, Northern Ireland, United atomic D or with the diatomic molecules HD and D2. Kingdom) The latter two cases are considered to be well under- stood through experimental and theoretical studies, Radiative association cross sections and rates are and the results have been implemented into astro- computed, using a quantum approach, for the for- chemical models. In contrast, the role of deuteration mation of C2 molecules (dicarbon) during the col- through reactions with atomic D remains an open lision of two ground state C(3P) atoms. We find question. Currently, astrochemical models rely on 1 3 that transitions originating in the C Πg, d Πg, and theoretical classical rate coefficients for these reac- 5 1 Πu states are the main contributors to the process. tions. Here, we present laboratory measurements of The results are compared and contrasted with pre- the rate coefficients for the reactions of atomic Dwith + + + vious results obtained from a semi-classical approx- H3 ,H2D , and D2H . The measurements were imation. New ab initio potential curves and transi- performed using a dual-source, merged fast beams tion dipole moment functions have been obtained for apparatus. Co-propagating beams allow us to mea- the present work using the multi-reference configu- sure absolute total cross sections for relative collision ration interaction approach with the Davidson cor- energies between ∼10 meV to ∼10 eV . In addition, rection (MRCI+Q) and aug-cc-pCV5Z basis sets, sub- high-level quantum ab initio calculations have been stantially increasing the available molecular data on carried out to model the zero-point-energy corrected dicarbon. Applications of the current computations energy profile and the shape of the potential energy to various astrophysical environments and labora- barrier, allowing an evaluation of tunneling effects.

129 From the combination of our experimental and the- 1 University of Minnesota (Minneapolis, Minnesota, United States) oretical results, we derive thermal rate coefficients in the temperature range relevant for prestellar cores. Flare-associated coronal EUV jets outline open mag- netic field lines providing an escaping path tothe for particles accelerated dur- 310 — Solar Physics Division ing solar flares. Several studies have shown an obser- Meeting (SPD), Flares III vational link between coronal jets (observed in EUV or soft X-rays) and type III radio bursts, produced by escaping beams of energetic electrons, or in-situ 310.01 — Probing the plasma sheet of the 2017 energetic electron events. In a few events, coronal September 10 limb event using microwave jets have also been associated with X-ray emitting en- spectroscopy ergetic electrons during flares. However, the likeli- Dale E. Gary1; Bin Chen1; Gregory D. Fleishman1; Gelu hood of the association of energetic electrons to coro- M. Nita1; Sijie Yu1 nal jets as well as the link between jet properties and 1 NJIT (Newark, New Jersey, United States) hard X-ray emission properties has not been investi- gated on a large sample of events. We present here In its later phases, the 2017 Sep 10 X8.2 limb flare a statistical study of the link between X-ray emitting produced a dramatic, nearly radial plasma sheet that energetic electrons and the associated coronal EUV was the site of both bi-directional radial flows (in- jets by looking at their relative timing, and their spa- ward and outward) and 100 km/s turbulent mo- tial and spectral characteristics. We observed non- tions measured in highly ionized Fe lines (Warren thermal electrons in only 1/4 of the jets and only et al. 2018). Below the plasma sheet is a dense set weak correlations between jets and flare properties. of post-reconnection flare loops whose upper loops These results will be discussed in the context of jet emit strongly in thermal hard X-rays and hot EUV modelling and particle acceleration and escape asso- lines (T ∼ 20 MK), while the lower loops emit in ciated with coronal jets. much cooler lines such as Ca II (Kuridze et al. 2019). Observations of gyrosynchrotron emission from the 310.03 — Thermal and Nonthermal Evolutions of a Expanded Owens Valley Solar Array (EOVSA) show Circular Ribbon Flare the presence of high-energy (> 300 keV) electrons at still higher heights above the EUV and hard X- Jeongwoo Lee1; Chang Liu2; Stephen M. White3; Haimin ray loops. At microwave frequencies above about 14 Wang2 GHz, EOVSA shows that the source shape is a nearly 1 Institute for Space Sciences, Shandong University (Weihai, complete loop while at frequencies below about 10 China) GHz, the source is split into two lobes on either side 2 New Jersey Institute of Technology (Newark, New Jersey, United of the plasma sheet. Using the spatially resolved States) EOVSA brightness temperature spectra, we investi- 3 Space Vehicles Directorate, Air Force Research Laboratory (Albu- gate the cause of this bifurcated spatial structure. querque, New Mexico, United States) There are two competing possibilities for the ”miss- ing” emission at lower frequencies: (a) the emis- We studied the activation and the extended activ- sion may be absorbed by intervening high-density, ity of a circular-ribbon flare, SOL2014-12-17T04:51 relatively cool material in the plasma sheet or (b) by performing the Differential Emission Measure the emission may be suppressed by the Razin ef- (DEM) inversion analysis of the extreme ultraviolet fect due to a combination of hot high density mate- (EUV) images of the Atmospheric Imaging Assem- rial and low magnetic field strength. We use diag- bly (AIA) instrument onboard the Solar Dynamics nostics from microwave imaging spectroscopy and Observatory (SDO) and analysis of the microwave AIA DEM analysis to determine the likely plasma data from the Nobeyama Radioheliograph (NoRH). parameters and other characteristics of the plasma We will present the following results. 1. The circular sheet, and the relative placement of the microwave- ribbon as an indicator of the dome-shaped separa- emitting electrons and the plasma sheet along the trix is better visible in the preflare phase in the form line of sight. of very narrow channel of enhance temperature. It is activated much earlier (10-15 min before the impul- 310.02 — Hard X-ray emitting energetic electrons sive phase at 04:33 UT), and its temporal correlation in connection with coronal EUV jets with the outer spine temperature suggests the initial activation of the circular ribbon by magnetic recon- Sophie Musset1; Mariana Jeunon1; Lindsay Glesener1 nection in the outer spine. 2. The flare ribbons are ac-

130 tive only within a limited section of the entire circu- to the loss of plasma confined in the rope and pro- lar ribbon, suggesting the hyperbolic flux tube recon- vide a viable explanation for coronal dimming and nection rather than null point reconnection. They are jet-like eruptions. Furthermore, the location of the activated 4 min before the impulsive phase together footpoints of the rope during the reconnections are with the inner spine, and involve nonthermal elec- found to be in good correlation with the dimming re- trons as evidenced by the NoRH 34 GHz emission. 3. gions inferred from Extreme-Ultraviolet images ob- The temperature-high region and the DEM-high re- served after the flare. gion coincide each other in the impulsive phase, and then separate from each other, implying that the ris- 310.05 — Radiative MHD Simulation of a Solar ing magnetic fields carry hot plasma away while the Flare high-density cooler plasma stays on the fan surface. 1 2 4. An unusually extended decay phase in this event Mark Cheung ; Matthias D. Rempel ; Georgios 1 2 3 can be understood as the maximum DEM in the im- Chintzoglou ; Feng Chen ; Paola Testa ; Juan Martinez- 1 1 1 pulsive phase occurs at a higher temperature and Sykora ; Alberto Sainz Dalda ; Marc L. DeRosa ; Anna 2 4 4 then gradually shifts to lower temperatures where Malanushenko ; Viggo Hansteen ; Mats Carlsson ; Bart 1 4 2 EUV emission is more efficient. Namely, the ex- De Pontieu ; Boris Gudiksen ; Scott W. McIntosh 1 tended EUV activity is due to slow cooling of the hot Lockheed Martin Solar and Astro Laboratory (Palo Alto, Califor- plasma within the confined magnetic structure. nia, United States) 2 High Altitude Observatory (Boulder, Colorado, United States) 3 310.04 — Magnetohydrodynamic Simulation of Harvard-Smithsonian Center for Astrophysics (Cambridge, Mas- sachusetts, United States) Magnetic Null-point Reconnections and Coronal 4 dimmings in NOAA AR 11283 University of Oslo (Oslo, Norway) We present a radiative MHD simulation of a solar Avijeet Prasad1; Karin Dissauer2; Qiang Hu1; Rami- 3 2 flare. The computational domain captures the near- tendranth Bhattacharyya ; Astrid Veronig ; Sanjay surface layers of the convection zone and overlying Kumar4; Bhuwan Joshi3 1 atmosphere. Inspired by the observed evolution of Center for Space Plasma & Aeronomic Research, The University NOAA Active Region (AR) 12017, a parasitic bipo- of Alabama in Huntsville (Huntsville, Alabama, United States) lar region is imposed to emerge in the vicinity of 2 Institute of Physics, University of Graz (Graz, Austria) 3 a pre-existing sunspot. The emergence of twisted Udaipur Solar Observatory, Physical Research Laboratory magnetic flux generates shear flows that create apre- (Ahmedabad, Gujrat, India) 4 existing flux rope underneath the canopy field ofthe Post Graduate Department of Physics, Patna University (Patna, sunspot. Following erosion of the overlying boot- Bihar, India) strapping field, the flux rope erupts. Rapid release of magnetic energy results in multi-wavelength syn- The magnetohydrodynamics of active region NOAA thetic observables (including X-ray spectra, narrow- 11283 is simulated using an initial non-force-free band EUV images, Doppler shifts of EUV lines) that magnetic field, extrapolated using the photospheric are consistent with flare observations. This works vector magnetogram of the active region. Particu- suggests the super-position of multi-thermal, super- larly, we focus on the magnetic reconnections (MRs) hot (up to ∼100 MK) plasma may be partially respon- occurring close to a magnetic null point that resulted sible for the apparent non-thermal shape of coronal in the X2.1 flare on 2011 September 06 around 22:12 X-ray sources in flares. Implications for remote sens- UT followed by the appearance of circular chromo- ing observations of other astrophysical objects is also spheric flare ribbons and coronal dimming. Impor- discussed. This work is an important stepping stone tantly, the extrapolated initial non-force-free field toward high-fidelity data-driven MHD models. shows the presence of a twisted flux rope near the polarity inversion line and a three-dimensional (3D) null situated near one of the major polarities. In the 310.06 — Multi-wavelength Investigation of simulated dynamics, we find MRs occurring below Energy Release and Chromospheric Evaporation the rope that leads to an increase in the twist and con- in Solar Flares sequent rise of the flux-rope. As one end of the ris- Viacheslav M. Sadykov1 ing rope approaches the 3D null point, reconnections 1 Physics, New Jersey Institute of Technology (Kearny, New Jersey, ensue – leading to the main flare and the subsequent United States) formation of circular flare ribbons. Interestingly, the MRs open up the flux-rope that can potentially lead For understanding of energy release and chromo- spheric evaporation in solar flares it is necessary to

131 perform a combined multi-wavelength analysis of observations. During the initial phase of an M6.5 observations from space- and ground-based obser- flare on 2015-06-22, two isolated emission patches vatories and compare the results with predictions are visible prior merging with the main flare rib- of the radiative hydrodynamic (RHD) flare models. bons. These two point sources are characterized with The case study of spatially-resolved chromospheric central reversals and significantly broadened Mg II evaporation for an M1.0-class solar flare using data k/h and C II Å lines, (with a FWHM of 1.6 Å and form IRIS, HMI/SDO, and VIS/GST, demonstrated 0.8 Å, respectively), respectively, likely due to tur- a complicated nature of evaporation and its connec- bulences. The Doppler shifts of optically thin lines, tion to the magnetic field topology. Following this Si IV 1402.77 Å and Mg II 2791.59 Å, suggest up- study, the Interactive Multi-Instrument Database of flows about 26 km/s and 2 km/s, respectively. A Solar Flares is designed for efficient search, integra- stand-alone EUV loop, connecting the two stationary tion, and representation of flares for statistical stud- flare footpoints, is identified by SDO/AIA images ies. Comparison of the energy release and chro- and confirmed by the coronal magnetic field extrap- mospheric evaporation properties for seven solar olated from the SDO/HMI magnetograms. The tem- flares simultaneously observed by IRIS and RHESSI poral variation of the intensity and differential emis- with predictions of the RHD electron beam-heating sion measure of the two brightenings show obvious flare models revealed weak correlations between de- delay, about 2-3 minutes, indicating localized recon- posited energy fluxes and Doppler shifts of IRIS nection and heating. In contrast, on the main flare lines for observations and strong for models, to- ribbon, the Si IV line shows obvious downflows with gether with other quantitative discrepancies. Statis- a speed of 38 km/s. The different behavior of the tical analysis of Soft X-Ray (SXR) emission, plasma flare ribbon and isolated footpoints is possibly due temperature (T), and emission measure (EM) proper- to the different heating magnitudes and altitudes. ties derived from GOES observations demonstrated that flares form two groups, “T-controlled” and 311.02 — Evolution of bipolar internetwork “EM-controlled”, distinguished by contribution of T magnetic fields and EM to the SXR peak formation and presumably evolving in loops of different lengths. Modeling of Milan Gosic1; Bart De Pontieu1; Luis Ramon Bellot the SDO/HMI LOS observables for RHD flare mod- Rubio2 els highlights that for high deposited energy fluxes 1 Lockheed Martin Solar & Astrophysics Lab (Palo Alto, California, (≥5×1010 erg cm−2s−1) the sharp magnetic transients United States) and Doppler velocities observed during the solar 2 Instituto de Astrofisica de Andalucia (IAA-CSIC) (Granada, flares by HMI should be interpreted with caution. Spain) Finally, the flare prediction problems and the role of the magnetic field Polarity Inversion Lines (PIL) Internetwork (IN) magnetic fields can be found in- in the initiation and development of flares are con- side supergranular cells all over the solar surface. sidered. The possibility to enhance the operational Thanks to their abundance and appearance rate, IN forecasts of M-class flares by considering jointly PIL fields are considered to be an essential contributor and other magnetic field and SXR characteristics is to the magnetic flux and energy budget of the so- demonstrated, with corresponding Brier Skill Score lar photosphere, and may also play a major role in (BSS=0.29±0.04) higher than for the SWPC NOAA the energy budget of the chromosphere and transi- operational probabilities (BSS=0.09±0.04). tion region. Therefore, it is crucial to understand how IN magnetic fields appear, evolve, interact with the preexisting magnetic structures, and what im- 311 — Solar Physics Division pact they have on the upper solar atmosphere. Here, Meeting (SPD), DKIST II we analyze spatio-temporal evolution of IN magnetic bipolar structures, i.e, loops and clusters, employing multi-instrument (IRIS and SST), multi-wavelength 311.01 — Chromospheric Evaporation Observed in observations of IN regions with the highest sensitiv- an Isolated Magnetic Flux Tube ity and resolution possible. For the first time, our Yan Xu1; Nengyi Huang1; Ju Jing1; Haimin Wang1 observations allow us to describe in detail how IN 1 NJIT (Newark, New Jersey, United States) bipoles emerge in the photosphere and even reach the chromosphere. We estimate the field strengths We study chromospheric evaporation of an isolated of these IN magnetic structures both in the photo- magnetic flux tube, with IRIS, SDO and BBSO/GST sphere and the chromosphere, using full Stokes mea-

132 surements in Fe I 6173 Å, Mg I b2 5173 Å, and Ca We report detailed observations of magnetic envi- II 8542 Å. Employing the IRIS FUV and NUV spec- ronment at four footpoints of two warm coronal tra, we show that IN fields contribute to the chromo- loops observed on 5 May 2016 in NOAA AR 12542 spheric and transition region heating through inter- (Loop I) and 17 Dec 2015 in NOAA AR 12470 (Loop action with the preexisting ambient fields. II). These loops were connecting a plage region with sunspot periphery (Loop I) and a sunspot umbra 311.03 — Disentangling Chromospheric (Loop II). We used Solar Dynamics Observatory Temperatures and Dynamics with ALMA and IBIS (SDO) and Goode Solar Telescope (GST) data to de- scribe the phenomenon and understand its causes. Kevin P. Reardon1; Momchil Molnar2; Yi Chai3; Ryan The study indicates loop brightening episodes were Hofmann2 associated with magnetic flux emergence and cancel- 1 National Solar Observatory (Boulder, Colorado, United States) lation processes observed in SDO’s Helioseismic and 2 APS, University of Colorado Boulder (Boulder, Colorado, United Magnetic Imager (HMI) and GST’s Near InfraRed States) Imaging Spectrapolarimeter (NIRIS) data. The ob- 3 New Jersey Institute of Technology (Newark, New Jersey, United served activity was driven by magnetic reconnec- States) tion between small-scale emerging dipoles and large- scale pre-existing fields, suggesting that the recon- The chromosphere is highly structured in density, nection occurred in the lower chromosphere at the dynamics, and temperature. Unfortunately, it can edge of an extended plage region, where the loops be difficult to disentangle the different contributions were rooted. We suggest that plasma, evaporated of these physical conditions to our current set of during these reconnection events, gradually filled observable diagnostics. With the advent of high- the loops and as it cooled the visible density front resolution observations of the millimeter continuum propagated from one footpoint of the loop to an- with the Atacama Large Millimeter Array (ALMA), other at a rate of 90-110 km/s. This study also in- we have a new tool to probe the chromospheric tem- dicates that at least some of the bright loops seen in perature structure. By combining these observa- SDO Atmospheric Imaging Assembly images rooted tions with similar observations in other visible, in- in sunspot umbra may be heated due to magnetic ac- frared, and UV lines, we are better able to disentan- tivity taking place at the remote (non-sunspot) foot- gle the thermal and dynamical behavior of the chro- point. mosphere. In this talk, we discuss the results of com- bining ALMA images with imaging spectroscopy from the Interferometric Bidimensional Spectrome- 312 — Plenary Lecture: ter (IBIS). We find evidence that spectral-line param- eters of Hα and Ca II are closely correlated with Cosmological Inference from the ALMA brightness temperatures. We have per- Large Galaxy Surveys, Elisabeth formed spectral inversions employing multiple diag- nostics to retrieve typical atmospheric conditions in Krause (University of Arizona) our field of view. We discuss how this joint analy- 312.01 — Cosmological Inference from Large sis changes our understanding of chromospheric dy- Galaxy Surveys namics and the interpretation of the observed spec- tral intensities. Finally, we explore how these results Elisabeh Krause1 can guide future observations of the chromosphere 1 University of Arizona (Tucson, Arizona, United States) from both ALMA and DKIST. The accelerated expansion of the Universe is the most 311.04 — Magnetic Field Dynamics and Varying surprising cosmological discovery in decades. It has Plasma Emission in Large Scale Coronal Loops inspired a new generation of ambitious surveys to determine the fundamental nature of this acceler- 1 2 3 Vasyl B. Yurchyshyn ; Seray Sahin ; Pankaj Kumar ; ation. I will introduce the different measurement 2 1 1 Ali Kilcik ; Kwangsu Ahn ; Xu Yang techniques used by today’s cosmologists, describe 1 Big Bear Solar Observatory, New Jersey Institute of Technology the landscape of current and near future wide-field (Big Bear City, California, United States) galaxy surveys, and present cosmology constraints 2 Physics, Akdeniz University (Antalya, Turkey) from the Dark Energy Survey (DES Y1). This analysis 3 NASA GSFC (Greenbelt, Maryland, United States) constrains the composition and evolution of the Uni- verse through a combination of galaxy clustering,

133 galaxy-galaxy lensing, and cosmic shear. These three generate cross sections even from huge line lists. Ex- measurements yield consistent cosmological results, oCross also allows facile conversion between ExoMol and in combination they provide some of the most and HITRAN formats. Work is in progress to pro- stringent constraints on cosmological parameters. I vide high accuracy transition frequencies for use in will describe the validation of measurements and high resolution studies of exoplanets. A formal im- modeling from pixels to cosmology and I will give plementation of this will form part of the 2020 Exo- an outlook on cosmology analysis plans and chal- Mol release. lenges for future, much larger experiments such as LSST and WFIRST. 314.02 — Latest updates to the CHIANTI atomic database 314 — Laboratory Astrophysics Peter R. Young2; Kenneth P. Dere1; Giulio Del Zanna3; Division Meeting (LAD): Bridging Enrico Landi4; Ralph Sutherland5 1 George Mason University (Washington, District of Columbia, Laboratory and Astrophysics: United States) Exoplanets III 2 NASA Goddard Space Flight Center (Greenbelt, Maryland, United States) 3 Cambridge University (Cambridge, United Kingdom) 314.01 — The ExoMol project: molecular line lists 4 University of Michigan (Ann Arbor, Michigan, United States) for the opacity of exoplanets and other hot 5 Australian National University (Weston Creek, Australian Capital atmospheres Territory, Australia) Jonathan Tennyson1 1 University College London (London, United Kingdom) CHIANTI is a database of atomic data parameters and a software package for computing the radia- The ExoMol project provides molecular line lists for tive emissions from optically-thin astrophysical plas- exoplanets and other atmosphere with a particular mas. CHIANTI is freely available to the community emphasis on those atmospheres which are signifi- (http://chiantidatabase.org), and is very widely cantly hotter than the Earth’s. ExoMol has now com- used in the Heliophysics and Astrophysics commu- puted line lists for over 40 molecules including, in nities. The papers describing CHIANTI have been most cases, isotopologues. These are available at cited over 3500 times in the 22-year lifetime of the www.exomol.com. Key new ine lists include ones for project. + TiO, H3 , NO, C2H4 and a significantly improved Version 9 of CHIANTI was released in March one for hot water, as well as for a range closed and 2019, and this presentation summarizes the new up- open shell diatomic molecules. dates and highlights important applications. The Fundamental molecular data play a key role for key change for CHIANTI 9 was the implementation spectral characterization of astrophysical objects cool of a new method to account for recombination and enough to form molecules in their atmospheres (cool dielectronic capture in the level balance equations stars, extrosolar planets and planetary discs) as well through new, two-ion models that fully capture the as in a broad range terrestrial applications. How- state-to-state transitions between ions. The models ever, at elevated temperatures, the laboratory data are needed for the calculation of X-ray satellite lines for a number of key species is absent, inaccurate or and, for the first time, enable density sensitivity tobe incomplete. The ExoMol project provides compre- modeled. hensive line lists with the aim of providing data for A number of the standard atomic data-sets have all molecules likely to be observable in exoplanet at- been updated, including recombination rates for sev- mospheres in the foreseeable future. This is a huge eral important coronal iron ions. New software rou- undertaking which involves providing in excess of a tines have been written for computing the differen- hundred of billion spectral lines for a large variety of tial emission measure of a plasma, and for comput- molecular species. ing the response functions of the Atmospheric Imag- The ExoMol database had a formal release in 2016; ing Assembly on board NASA’s Solar Dynamics Ob- it provides information on a variety of topics in- servatory . cluding, of course, line lists, cross sections (gener- ated from the same line lists), lifetimes and Landé g-factors. It comprises 52 molecules (130 isotopo- logues). Our new flexible code ExoCross can rapidly

134 314.03 — Lifetimes, Branching Fractions, and Structure Packages, Grasp0[1, 4] and Grasp2K[2], are Oscillator Strengths for Ultraviolet Transitions in used to obtain the level energies and transition prob- P II and Cl I abilities. Here, Au III, as well as its low-charged iso- electronic sequence members, Ir I, Pt II, and Hg IV, Steven Robert Federman1; Rabee Alkhayat1; Michael 1 1,2 1 are computed and compared against available theo- Brown ; Negar Heidarian ; Richard Irving ; Jeremy retical and experimental data[3]. The Au III results Bancroft Brown1; Song Cheng1; Larry Curtis1; David 1 are used to simulate the emission spectrum to inter- Ellis pret the Compact Toroidal Hybrid experiment with 1 Univ. of Toledo (Toledo, Ohio, United States) 2 a gold-plated probe. This work was partially sup- Univ. of Maryland (College Park, Maryland, United States) ported by NSF grant 1816984. [1] Dyall, et al., Computer physics communica- Observations of absorption from ultraviolet transi- tions, 55(3):425–456, 1989. [2] Per Jonsson, et al., tions of atomic species in diffuse interstellar clouds Computer Physics Communications, 184(9):2197– provide data on elemental gas phase abundances. 2203, 2013. [3] Kramida, et al. NIST Atomic Spec- From this information the level of depletion onto in- tra Database, https://physics.nist.gov/asd [4] terstellar grains, the nucleosynthetic pathways for Parpia, et al., Computer physics communications, the element, and the chemistry involving the element 94(2-3):249–271, 1996 can be inferred. Here we describe results on P II and Cl I from beam-foil measurements with the Toledo Heavy Ion Accelerator that build on our earlier ef- 315 — WFIRST Ultra-Deep Fields forts on P II λ1153 and Cl I λλ1088, 1097, 1347. In par- ticular, lifetimes, branching fractions, and the associ- II ated oscillator strengths (f -values) for the P II multi- plet at 1308 Å and for Cl I lines at 1004, 1079, 1090, 315.01 — Deep Grism/Prism observations with and 1095 Å were obtained. Contamination from P I WFIRST and P IV emission had to be removed for an accurate Sangeeta Malhotra1 set of P II branching fractions. Our results for the 1 NASA Goddard Space Flight Center (Tempe, Arizona, United suite of transitions in P II and Cl I agree very well States) with the data obtained from recent theoretical cal- culations, and our f -values for the Cl I lines confirm Multiple projects on HST have shown the usefull- the values inferred from spectra acquired with the ness of deep slitless grism spectroscopy. The main Far Ultraviolet Spectroscopic Explorer. Future analyses advantage is to get spectra of everything in an un- of interstellar P and Cl abundances can be placed on biased way. This has led to studies of emission line a more secure footing. dominated galaxies, which would not make the spec- troscopy cut on the basis of continuum brightness 314.04 — Relativistic Atomic Structure of the Au alone. These are low mass, low metallicity star- III Isoelectronic Sequence: opacity data for burst galaxies. Even without emission lines these kilonova ejecta spectra can be used to improve and calibrate pho- tometric redshifts. Deep spectroscopy observations 1 1 1 Yier Wan ; Z. S. Taghadomi ; A. Flowers ; Phillip by WFIRST can provide a few 100,000 redshifts per 1 4 2 C. Stancil ; Brendan M. McLaughlin ; S. Loch ; S. WFIRST field, including those of Lyman-α and Ly- 3 3 3 Bromley ; J. P. Marler ; C. E. Sosolik man Break galaxies in the epoch of reionization. 1 The University of Georgia (Athens, Georgia, United States) 2 Auburn University (Auburn, Alabama, United States) 3 315.02 — Deep Fields, PFS, and Other Clemson University (Clemson, South Carolina, United States) Spectroscopic Surveys 4 Queen’s University (Belfast, United Kingdom) Rachel Bezanson1 The detection of a neutron star merger (NSM) event 1 University of Pittsburgh (Pittsburgh, Pennsylvania, United and the spectral observation of its optical and in- States) frared emission opens up the possibility of direct in- terrogation of the formation site of heavy r-process I will discuss existing and planned spectroscopic sur- elements. However, laboratory spectroscopic data veys in the context of ancillary datasets in potential for the vast range of heavy elements are severely lim- WFIRST deep fields. In particular, I will focus onthe ited. The current focus is on one of the “second peak” wide field PFS galaxy evolution spectroscopic sur- elements - gold. Two General Relativistic Atomic vey - describing the multi-wavelength photometric

135 data and optical/NIR spectroscopic targeting strate- source modeling and source separation by working gies and anticipated data quality. on multi-band and images and by combining im- ages of different resolution (both spatially and spec- 315.03 — Constraining the Evolution of trally). It is specifically developed for joint pixel- Reionization with US-ELT Followup of WFIRST level processing of data from LSST, WFIRST, and Eu- Deep Drilling Fields clid and leverages their imagers and grism spectro- graphs. I will introduce the method, discuss the sta- 1 Steven L. Finkelstein tistical challenges in interpreting scenes consistently 1 University of Texas (Austin, Texas, United States) across multiple data sets, and demonstrate the im- provement for precision measurements and astro- The epoch of reionization (6 < z < 10) marks the physical modeling that are achievable with SCAR- period in our universe when the first large galax- LET. ies grew to fruition, and began to affect the uni- verse around them. Massive stars, and potentially accreting supermassive black holes, filled the uni- 316 — ISM & The Milky Way verse with ionizing radiation, burning off the haze of neutral gas that had filled the intergalactic medium 316.01 — Critical Ionization Velocities in (IGM) since recombination (z ∼ 1000). The evolu- Interstellar Space: An Introduction tion of this process constrains key properties of these 1 earliest luminous sources, thus observationally con- Gerrit L. Verschuur 1 straining reionization is a key science goal for the Unaffiliated (Sunnyvale, California, United States) next decade. The measurement of Lyα emission The critical ionization velocity (CIV) is a well-studied from photometrically-identified galaxies is a highly plasma phenomenon where atoms become ionized constraining probe of reionization, as a neutral IGM in the presence of a magnetic field when their kinetic will resonantly scatter these photons, reducing de- energy relative to plasma is equivalent to their ion- tectability. While significant work has been done ization potential. This effect has been observed in the with 8–10m telescopes, these observations require ex- laboratory and in near-earth space and is the subject tremely large telescopes (ELTs) – the flux limits avail- of an extensive literature. We will briefly outline the able from today’s 10m class telescopes are sufficient process by which ionization is facilitated. The signa- for only the brightest known galaxies (m < 26). Ultra- ture of this effect is found in the component structure deep surveys with the Giant Magellan Telescope of interstellar neutral hydrogen emission profiles ob- (GMT) and Thirty Meter Telescope (TMT) will be tained as part of the GALFA HI Survey. This is dra- capable of detecting Lyα emission from galaxies 2- matic confirmation of similar results based on anal- 3 magnitudes fainter than today’s deepest surveys. ysis of earlier studies of HI profiles obtained with Wide-field fiber spectroscopy on the GMT combined other telescopes. The CIV phenomenon, mediated with narrow-field AO-assisted slit spectroscopy on by plasma instabilities, may act as a major source of the TMT will be able to probe the expected size energy in the interstellar medium, a conclusion that of ionized bubbles throughout the epoch of reion- has far-reaching consequences for our understand- ization, following up ∼degree scale deep imaging ing of interstellar physics. surveys with the Wide Field Infrared Space Telescope. These data will provide the first resolved Lyα-based 316.02 — Hydrogen, Helium, and Magnetic Fields maps of the ionized intergalactic medium through- in Interstellar Space out the epoch of reionization, constraining models of both the temporal and spatial evolution of this phase Joan T. Schmelz1; Gerrit L. Verschuur2 change. 1 USRA (Columbia, Maryland, United States) 2 Unaffiliated (None, California, United States) 315.04 — Modeling the Sky with All Available Analysis by multiple authors of a variety of inter- Data stellar neutral hydrogen features studied over many Peter Melchior1 decades using data from different telescopes reveals 1 Princeton University (Princeton, New Jersey, United States) a pervasive 34 km/s wide component. The tradi- tional explanation, that the line width results from The image modeling framework ”SCARLET” (Mel- a kinetic temperature, would mean that T = 24,000 chior et al. 2018) enables the joint use of multiple K, high enough to ionize the gas so it could not con- data sets of the same celestial scene. It improves tribute to the 21-cm profile. Turbulent motions could

136 explain a pervasive broad component, but not why to, which requires further study to confirm) turbu- it has the same numerical value in so many different lent energy and create slightly super-Alfvénic cores types of HI features. Confusion due to telescope side out of sub-Alfvénic clouds. The results of our sim- lobes has been proposed as a possible explanation, ulations also agree with the observed velocity-scale, but the broad feature persists in side-lobe-corrected mass-scale, and field-density relations. survey data. The critical ionization velocity is a well- studied plasma phenomenon where atoms become 316.04 — On the Search for ionized in the presence of a magnetic field when their Signs of Intelligent Life Near the Galactic Center kinetic energy relative to the plasma is equivalent to 1 1 1 the ionization potential. The critical ionization ve- Vishal Gajjar ; Andrew Siemion ; Steve Croft ; David 1 1 1 locity for helium is 34 km/s, which could account R. DeBoer ; J. Emilio Enriquez ; Howard T. Isaacson ; 1 1 1 for the pervasiveness of this component. This re- Matt Lebofsky ; David MacMahon ; Daniel Price ; Dan 1 sult supports other evidence that the neutral hydro- Werthimer 1 gen in the interstellar medium is tightly coupled to Department of Astronomy, University of California (Albany, the galactic magnetic field (Clark et al. 2014; 2015). California, United States) Strong support for this interpretation stems from the resulting abundance of interstellar helium, which Over the last decade, discoveries of numerous earth can be estimated from the column density fraction type exoplanets have extended the possibility of of the 34 km/s component with respect to the entire other life-bearing worlds. However, the question emission profile. A derived value of 0.28 is within of the existence of intelligent life might remain elu- one σ of the cosmic abundance of helium. sive unless a dedicated attempt is made to exten- sively Search for Extra-Terrestrial Intelligence (SETI). The Breakthrough Listen (BL) is a 10-year effort to 316.03 — Anchoring Magnetic Fields in Turbulent conduct the most sensitive, comprehensive, and in- Molecular Clouds. II. From 0.1 to 0.01 pc tensive search for advanced intelligent life on other Yapeng Zhang1 worlds ever performed. The Galactic Center (GC) is 1 Physics, The Chinese University of Hong Kong (Hong Kong, a key observational target for the radio component Hong Kong) of the BL program. The line of sight toward the GC offers the largest integrated galactic star count ofany We compared the magnetic field directions inferred direction in the sky, is a widely cited possible loca- from polarimetry data obtained from 100 pc scale tion for beacon builtby an advanced intelligence and inter-cloud media (ICM) and from subparsec scale is the most energetic region in the Milky Way. Given molecular cloud cores. The highly correlated re- the potential for discovery in the GC region, the BL sult led us to conclude that cloud turbulence must survey will cover the entire frequency range from 700 be sub-Alfvénic. Here we extend the study with MHz to 100 GHz using the Green Bank Telescope 0.01 pc cores observed by interferometers. The in- (GBT) and Parkes Telescope. We plan to conduct ferred field directions at this scale significantly de- deep observations of around 350 hours from the GBT viate from that of the surrounding ICM. An obvious and 280 hours from the Parkes telescope; making it question to ask is whether this high-resolution result the most significant SETI survey to date of any region contradicts the sub-Alfvénic picture concluded ear- of the sky. The GC region is also an exciting observa- lier. We performed MHD simulations of a slightly tional target for a host of natural astrophysical phe- super-critical (magnetic criticality = 2) clouds with nomena, prominently including pulsars in close or- Alfvénic Mach number M퐴= 0.63 (MA ≡ < σV /VA bits around the central super-massive black hole, Sgr >, where σV and VA are, respectively, local 3D ve- A, or in new exotic systems such as a millisecond pul- locity dispersion and Alfvén velocity; < ... > means sar in a binary system with a black hole. Other astro- the average within the entire simulated volume; e.g., physics of interest include accelerated masers, spec- Burkhart et al. 2009), which can reproduce the Pa- tral line surveys, and studies of the detailed struc- per I results, and observed the development toward ture of the dense ionized Interstellar Medium (ISM) smaller scales. Interestingly, all subregions hosting in the GC. I will review these observation strategies 5 cores with n(H2) > 10 /cc (the typical density ob- and novel data analysis techniques we plan to deploy served by interferometers) possess MA = 2–3. Not to investigate a range of signal types using state-of- too surprisingly, these slightly super-Alfvénic cores the-art machine learning tools. result in B-field orientation offsets comparable tothe interferometer observations. The result suggests that gravity can concentrate (and maybe also contribute

137 316.05 — The Spiral Magnetic Field in the Central infrared spectrographs were analysed using Markov 5 Parsecs of the Galaxy Chain Monte Carlo techniques that simultaneously

1 2 fit for the radial velocity, Teff, vsini, and veiling by C. Darren Dowell ; David T. Chuss ; Jordan A. comparison with synthetic spectra. The radial ve- Guerra2; Martin Houde3; Joseph M. Michail2; Mark 4 5 6,7 locity distribution for 32 objects, most with Class Morris ; Joan T. Schmelz ; Johannes Staguhn ; I or Flat-spectrum spectral energy distributions, is Michael W. Werner1 1 marginally gaussian, with a higher dispersion rela- Jet Propulsion Laboratory, California Institute of Technology tive to optical surveys at the 2 σ level. When com- (Pasadena, California, United States) 2 paring the results from both proper motion and ra- Villanova University (Villanova, Pennsylvania, United States) dial velocity surveys in L 1688, there is a trend for 3 University of Western Ontario (London, Ontario, Canada) 4 the 1-D dispersions to be higher for samples of Class University of California, Los Angeles (Los Angeles, California, I/Flat-spectrum young stellar objects that reside in United States) 5 the cloud core compared to Class II/III dominated SOFIA/USRA (Mountain View, California, United States) samples which are located in the lower extinction 6 Johns Hopkins University (Baltimore, Maryland, United States) 7 periphery. In addition, there is a velocity gradient NASA/Goddard Space Flight Center (Greenbelt, Maryland, along the major axis of the cloud core that appears United States) more pronounced than that derived from optically visible objects at the cloud edges. If these higher dis- At λ ≈ 50 microns, the most prominent feature in the persions for Class I/Flat-spectrum objects are con- inner parsecs of the Milky Way is the rotating, irreg- firmed by future surveys, this could imply a super- ular Circum-Nuclear Ring (CNR) which demarcates virial state for the less evolved objects in the cloud the inner boundary of the molecular gas that is likely core and be a signature of the initial collapse and re- spiraling in toward the supermassive black hole. The bound of the cluster as suggested by recent simula- gas is magnetized, with previous estimates of field tions of cluster evolution. strength exceeding 1 milliGauss. We present new ob- servations of the polarization and inferred magnetic field structure of the CNR and vicinity, made atλ= 317 — Solar Physics Division 53 microns with the HAWC+ instrument on SOFIA. These observations show a spiral magnetic field on Meeting (SPD), Eruptions scales of 0.5 - 5 pc, with organized components, but mostly lacking the 180 degree symmetry of existing 317.01 — A Two-Sided-Loop X-Ray Solar Coronal magnetized accretion disk models. We discuss esti- Jet and a Sudden Photospheric Magnetic-field mates of the magnetic field strength from the 53 mi- Change, Both Driven by a Minifilament Eruption cron data, the relationship of these data to observa- Alphonse C. Sterling1; Louise Harra2; Ronald L. Moore3; tions at shorter and longer far-infrared wavelengths, David Falconer3 and interpretation of several of the magnetic features 1 NASA/MSFC (Huntsville, Alabama, United States) observed. 2 PMOD/WRC, ETH-Zurich (Zurich, Switzerland) 3 UAH/CSPAR, NASA/MSFC (Huntsville, Alabama, United 316.06 — A Radial Velocity Survey of Embedded States) Sources in the Rho Oph Molecular Core Most of the commonly discussed solar coronal jets Bruce A. Wilking1; Timothy Sullivan1; Thomas P. are of the type consisting of a single spire extending Greene2; Lindsey Lisalda3; Erika L. Gibb1; Chemeda approximately vertically from near the solar surface Ejeta1 into the corona. Recent research shows that erup- 1 Univ. of Missouri, St. Louis (Saint Louis, Missouri, United tion of a miniature filament (minifilament) drives at States) least many such single-spire jets, and concurrently 2 NASA Ames Research Center (Moffet Field, California, United generates a miniflare at the eruption site. A different States) type of coronal jet, identified in X-ray images dur- 3 Washington University in St. Louis (St. Louis, Missouri, United ing the Yohkoh era, are two-sided-loop jets, which States) extend from a central excitation location in oppo- We present the results of a radial velocity survey of site directions, along two opposite low-lying coro- young stellar objects in early stages of evolution in nal loops that are more-or-less horizontal to the sur- the core of the L 1688 molecular cloud. New and face. We observe such a two-sided-loop jet from the archival spectra obtained with four high resolution edge of active region (AR) 12473, using data from

138 Hinode XRT and EIS, and SDO AIA and HMI. Sim- 317.03 — STITCH: A New Method for Generating ilar to single-spire jets, this two-sided-loop jet re- Filament Channels and Driving Solar Eruptions sults from eruption of a minifilament, which acceler- Joel Dahlin1; Spiro K. Antiochos2; C. Richard DeVore2 ates to over 140 km/s before abruptly stopping upon 1 striking overlying nearly-horizontal magnetic field at Universities Space Research Association (College Park, Maryland, United States) ∼30,000 km altitude and producing the two-sided- 2 loop jet via interchange reconnection. Analysis of NASA/GSFC (Greenbelt, Maryland, United States) EIS raster scans show that a hot brightening, consis- We present a new formalism for generating eruptive tent with a small flare, develops in the aftermath of magnetic structure in MHD simulations of the solar the eruption, and that Doppler motions (∼40 km/s) corona. STITCH (STatistical InjecTion of Condensed occur near the jet-formation region. As with many Helicity) derives from the helicity condensation single-spire jets, the trigger of the eruption here is model of Antiochos (2013). In the helicity conden- apparently magnetic flux cancelation, which occurs sation model, small-scale photospheric convection at a rate of ∼4×1018 Mx/hr, comparable to the rate drives a reconnection-mediated inverse cascade that observed in some single-spire AR jets. An apparent concentrates energy and structure to form highly increase in the (line-of-sight) flux occurs within min- sheared filament channels.Our recent 3D MHD cal- utes of onset of the minifilament eruption, consistent culations using more than 100 cyclonic surface flows with the apparent increase being due to a rapid re- have demonstrated explosive solar eruptions driven configuration of low-lying magnetic field during the by helicity condensation. However, this manner of minifilament eruption. Details appear in Sterling et direct calculation of small-scale flows and the result- al. (2019, ApJ, 871, 220). ing reconnection is prohibitively expensive for use in data-driven event modeling or long-duration mag- 317.02 — New Insights into the 10 September 2017 netofrictional studies of the global solar magnetic Mega-Eruption field (Mackay et al. 2014, 2018). Our new method, STITCH, directly injects the tangential field (shear) 1 3 1 Judith T. Karpen ; Pankaj Kumar ; Spiro K. Antiochos ; resulting from statistically averaged, sub-grid he- 2 3 Dale E. Gary ; Joel Dahlin licity condensation. Numerically, this represents a 1 NASA GSFC (Greenbelt, Maryland, United States) source term in the induction equation, consisting of 2 NJIT (Newark, New Jersey, United States) the curl of the vertical field times a factor propor- 3 USRA (Greenbelt, Maryland, United States) tional to the cyclonic specific angular momentum -a single free parameter. The new approach reproduces The X8.2 flare on 10 September 2017 was part of prior calculations with small-scale flows at greatly a well-observed, extremely energetic solar eruption reduced computational expense. We present a va- that has been intensely studied. Much attention has riety of simulations with complex initial flux distri- been devoted to the striking appearance and persis- butions to demonstrate the flexibility of the model. tence of a current sheet behind the explosively accel- STITCH is both simple to implement and computa- erating CME. We focus here on the unusual appear- tionally inexpensive, making it a useful new tech- ance of prominent emission features on either side of nique for event-based and data-driven modeling of the flare arcade, which were detected in microwave solar eruptions. This work was supported by the emissions by NJIT’s EOVSA before the peak impul- NASA LWS, NPP, H-SR and ISFM programs. sive phase. Our analysis combines the results of 3D numerical simulations with observations by SDO, 317.04 — Bounding the Energy of Solar Eruptions EOVSA, and IRIS to decipher the underlying mag- netic structure of the erupting region and the initia- Jon A. Linker1; Cooper Downs1; Ronald M. Caplan1; tion mechanism. The event originated in a complex Tibor Torok1; Pete Riley1; Viacheslav Titov1; Roberto active region with a large-scale quadrupolar mag- Lionello1; Zoran Mikic1; Tahar Amari1 netic field punctuated by many intrusions of minor- 1 Predictive Science Inc (San Diego, California, United States) ity polarity. We interpret the observed microwave features as evidence of electron acceleration due to Major solar eruptions such as X-class flares and breakout reconnection, and present compelling evi- coronal mass ejections (CMEs) are the fundamental dence for this conclusion. source of solar energetic particles and geomagnetic storms, and are thus key drivers of space weather at Earth. The energy for solar eruptions is recognized to originate in the solar magnetic field, and is be- lieved to be stored as free magnetic energy (energy

139 above the potential field state) prior to eruption. So- (M1 or greater). We present MAG4’s improvement lar active regions are the site of the most violent ac- in forecasting SPEs (Solar Particle Events) and X-class tivity. Solar active regions can store widely varying flares as well. The improvement in forecasting CMEs amounts of energy, so knowledge of the free energy will be evaluated in the future. These new forecast- alone does not necessarily tell us when an eruption ing curves are being implemented in the near-real- is imminent. For estimates of the free energy to pro- time operational MAG4, though forecasts from the vide predictive power, we must know how much en- old curves will still be given. This work is funded by ergy a region can store - what is the energy bound? NSF’s Solar Terrestrial Program, and NASA/SRAG. In recent work, we have found that the energy of a particular field, the partially open field (POF), can 317.06 — A statistical study of magnetic flux ropes place a useful bound on the energy of an eruption in the solar active region with strong from real active regions, a much tighter constraint non-neutralized current than the energy of the fully open field. However, in 1 2 1 general, it is difficult to solve for the POF. In this pre- Wensi Wang ; Jiong Qiu ; Rui Liu 1 sentation, we discuss methods for approximating the Department of Geophysics and Planetary Sciences, University of energy of this field, and show a comparison of the ap- Science and Technology of China (Hefei, Anhui, China) 2 proximation for a case where the solution is known. Montana State University (Bozeman, Montana, United States) We discuss the implications for understanding and predicting major solar eruptions. Recent studies suggest non-neutralized electric cur- Research supported by NASA and AFOSR rent in the active region may relate to the solar erup- tions. Our previous studies show that the footpoints of the pre-existing magnetic flux rope (MFR) is co- 317.05 — Improving Forecasting of Drivers of spatial with strong non-neutralized current, while Severe Space Weather with the New MAG4 HMI the in-situ formed MFR is not. These results imply Vector Magnetogram Database that strong non-neutralized current in the MFR’s feet David Falconer1; Sanjiv Tiwari2; Ronald Moore1; Megan may relate to the eruptions. In this study, we in- Fisher3 tend to test whether strong current will be one sig- 1 CSPAR, UAH (Huntsville, Alabama, United States) nature of pre-existing MFRs and whether it relate 2 Lockheed Martin (Palo Alto, California, United States) to the eruptions. We investigate 10 active regions 3 Wooster College (Wooster, Ohio, United States) with strong non-neutralized currents. All active re- gions are characterized by strong shear motions or Major solar flares and Coronal Mass Ejections sunspot rotations. We found 13 MFRs, which ap- (CMEs) are drivers of severe space weather. The pear as expanding structures, filaments, sigmoids, or strongest ones come from active regions (ARs). They hot channels before/during their eruption. The foot- are powered by explosive release of magnetic en- points of MFRs are identified unambiguously with ergy. MAG4 (Magnetogram Forecast) is a large- conjugate coronal dimmings. The results show that database near-real-time tool that measures an AR’s the MFRs with clear pre-eruption dimmings are co- free-energy proxy from the AR’s deprojected HMI spatial with strong currrents. However, half of MFRs vector magnetograms. MAG4 converts the free- only with post-eruption dimmings are not in strong energy proxy to the AR’s predicted event rate (and currents regions. We also found most pre-eruption event probability) using a forecasting curve. MAG4 dimmings are co-spatial with sunspot rotation, while forecasts the event rate and probability for each post-eruption dimmings that relate to strong cur- AR on the disk, as well as for the full disk. The rents are co-spatial with shear motion regions. forecasting curves presently used by MAG4 are de- rived from a large sample of SOHO/MDI AR mag- netograms. This requires the HMI vector magne- 318 — Solar Physics Division tograms to be degraded in spatial resolution to ap- proximate what MDI would have measured, in or- Meeting (SPD), Helioseismology der to use the MDI forecasting curves. We report & Interior on the improved performance of MAG4 that results from using forecasting curves based on MAG4’s new 318.01 — On the latitude dependence of Rossby database of HMI vector magnetograms instead of us- waves in the Sun ing the present forecasting curves that are based on 1 1 MDI line-of-sight magnetograms. MAG4’s forecast- Bastian Severin Niklas Proxauf ; Laurent Gizon ; Björn 1 1 1 ing skill score significantly improves for major flares Löptien ; Jesper Schou ; Aaron C. Birch ; Richard S.

140 Bogart2 first and second kind) to characterize poleward and 1 Solar and Stellar Interiors, Max Planck Institute for Solar System equatorward wave propagation in spherical coordi- Research (Göttingen, Lower Saxony, Germany) nates. For this study we have developed control pro- 2 W. W. Hansen Laboratory, Stanford Uni- cedures which assess and remove center-to-limb arti- versity (Stanford, California, United States) facts, using measurements obtained by applying the procedure to pseudo poles at the east and west limbs. We study the latitude and depth dependence of so- Forward modeling is carried out to evaluate the con- lar Rossby waves. We use horizontal flows from lo- sistency of the corrected LFD frequency shifts with cal helioseismology (ring-diagram analysis) at dif- various assumed models of the depth variation of the ferent depths in the solar interior. From these we meridional circulation. compute maps of the radial vorticity. We confirm DB is supported by the NASA Heliophysics Divi- the existence of solar Rossby waves in the sectoral (m sion (awards 80NSSC18K0066 and 80NSSC18K0068) = l) power spectra at all depths down to 17 Mm be- and by the Solar Terrestrial program of the National low the surface. The depth dependence of the eigen- Science Foundation (award AGS-1623844). functions is consistent with rm, although this is a weak constraint due to the noise level. The latitu- 318.03 — Exploring the Coexistence of Two dinal eigenfunctions are observed to be more nar- m Distinct Dynamo States in the Sun through row than |sin(θ)| , likely indicating that the modes Global Simulations sense the latitudinal differential rotation. Further- more, we detect a non-zero imaginary component Loren Matilsky1; Juri Toomre1 of the latitudinal eigenfunctions, possibly related to 1 Astrophysical and Planetary Sciences, University of Colorado viscous dissipation. These new observations provide Boulder & JILA (Boulder, Colorado, United States) additional constraints on the physics of large-scale Rossby waves in the Sun. The origin of the Sun’s magnetism remains one of the most pressing outstanding problems in solar physics. 318.02 — Probing the Variation with Depth of the The number of sunspots (eruptions of magnetic flux Solar Meridional Circulation using Legendre through the photosphere) rises and falls over a reg- Function Decomposition ular 11-year cycle. Within each cycle, the sunspots emerge at mid-latitudes near and Douglas Braun1; Aaron C. Birch2; Yuhong Fan3 then closer to the equator as the cycle progresses. 1 NWRA (Boulder, Colorado, United States) Furthermore, the polarity sense of sunspot pairs is 2 Max Planck Institute for Solar System Research (Göttingen, Ger- opposite in the Northern hemisphere compared to many) the Southern hemisphere, and this polarity sense 3 High Alitude Observatory, National Center for Atmospheric flips from one 11-year cycle to the next. Recently, 3D, Research (Boulder, Colorado, United States) global, MHD dynamo simulations have made sub- stantial contact with observations, yielding regular The solar meridional circulation is a crucial compo- cycling, polarity reversals, and in a few cases, equa- nent of magnetic flux transport and dynamo mod- torward propagation of interior magnetic field. Here els. Despite decades of helioseismic study, no con- we present a new class of 3D, global simulations of sensus exists regarding the variation of its properties a solar convection zone that remarkably achieve two with depth. It has become apparent that the main distinct states of the dynamo coexisting simultane- challenges consist of 1) overcoming realization noise ously. One state consists of two opposite-polarity with multi-year long datasets, and 2) the identifica- reservoirs of magnetism in each hemisphere that cy- tion and robust removal of systematic center-to-limb cle, flip polarity, and exhibit equatorward propaga- effects. Here we apply the helioseismic methodol- tion, in remarkable agreement with the observed so- ogy of Legendre Function Decomposition (LFD) to lar cycle. Superimposed is another state, asymmet- 7.5 years of Dopplergrams obtained by the Helio- ric about the equator, that consists of one reservoir seismic and Magnetic Imager (HMI) as the basis of of strong toroidal field in a single hemisphere that inferring the depth variation of the meridional flow flips polarity and migrates poleward with the cy- between 20 and 60 degrees latitude in both hemi- cle, in agreement with many other dynamo simula- spheres. The LFD method, first developed by Braun tions. We describe theoretically how our simulated and Fan in 1998, probes subsurface flows through dynamos might be achieved and whether such pro- the Doppler-effect induced distortion of power spec- cesses could be at work in the solar dynamo. We also tra. The procedure is optimized for the detection of investigate the possible observable signatures of two meridional flows and uses Legendre functions (of the

141 distinct dynamo states if they were present in the so- that the work done by Lorentz force is the source lar interior. of magnetic energy inside the solar convection zone and the feedback of this Lorentz force on plasma ex- 318.04 — Deriving Three-Dimensional Sensitivity plains the reduction of latitudinal shear in differen- Kernels for Large-Scale Solar Interior Flows Using tial rotation when magnetic field is being inducted. Wavefield Simulations During the two solar minima covered by the mea- surements, the differential rotation of the Sun was in 1 2 Junwei Zhao ; Thomas Hartlep the state of highest latitudinal shear which reduced 1 Stanford Univ. (Stanford, California, United States) during the rising phase of sunspot cycles and replen- 2 Bay Area Environmental Research Institute (Moffett Field, Cali- ished during their declining phase. This suggests fornia, United States) that the baseline differential rotation profile of the Sun is its profile near solar minimum, not the rota- At present, a common method for inferring the Sun’s tion profile obtained by calculating its mean rotation interior meridional-circulation profile is to invert he- rate over a sunspot cycle. lioseismically measured travel-time shifts using sen- We have also developed a significantly improved sitivity kernels. The sensitivity kernels describe how local correlation tracking algorithm for tracking much travel-time shifts are expected, caused by a magnetic features on the solar surface from line-of- flow at a certain interior location, at each surface sight magnetograms by removing several systematic measurement distance. Ray-approximation kernels, effects like peak-locking, center-to-limb effect, etc. despite their shortcomings, have been used by many The new algorithm can detect shifts as small as 0.04 authors and provided tremendous insight into the pixel whereas the original algorithm detected shifts solar interior. In the meantime, more realistic global- larger than 0.2 pixels reliably. The measurements of scale Born-approximation kernels have been devel- large scale meridional flow and differential rotation oped by some authors. Here, we introduce a new ap- on the solar surface obtained from line-of-sight mag- proach for deriving three-dimensional flow kernels. netograms of MDI (1995-2011) and HMI (2010-2019) We perform global-Sun wavefield simulations with using the new algorithm suggest that the amplitude small flow perturbations placed at pre-determined of meridional flow is anti-correlated with sunspot locations inside the simulated Sun, and measure the number. These large scale flow patterns serve as vi- travel-time shifts they cause. A set of linear equa- tal inputs for solar dynamo models and have impli- tions links the flow model, which we prescribe, and cations for the prediction of the solar magnetic cycle. the travel-time shifts, which we measure from the simulated data, with the sensitivity kernels. By com- 318.06 — The Relationship Between Differential puting many such simulations, with perturbations at Rotation and Constant Effective Temperature in many different depths and locations relative tothe the Sun wave source, this set of linear equations can be suc- cessfully solved numerically for the sensitivity ker- Loren Matilsky1; Bradley W. Hindman1; Juri Toomre1 nels. 1 Astrophysical and Planetary Sciences, University of Colorado Boulder & JILA (Boulder, Colorado, United States) 318.05 — Observational Constraints on the Solar Helioseismology has shown that the rotation rate of Dynamo the solar interior is constant along radial lines (coni- Sushant Sushil Mahajan1 cal rotation contours) and has a mostly uniform gra- 1 Physics & Astronomy, Georgia State University (College Park, dient from equator to pole, facts which are still not Maryland, United States) completely understood. Conical rotation contours and uniform rotation gradients have been repro- Our analysis of helioseismic measurements of rota- duced in previous global, 3D, hydrodynamic simu- tion rate in the solar interior show that latitudinal lations of the solar convective envelope by imposing shear in differential rotation of the lower half of the a small temperature gradient at the base of the con- convection zone is anti-correlated with the sunspot vective layer, consistent with thermal wind balance number. This is evidence for Parker’s Ω-effect which in the tachocline. Here we show that similar results proposes that the latitudinal shear is responsible for can be obtained in global simulations by demanding amplifying the sunspot producing toroidal field. Us- that the conductive flux through the outer boundary ing the basic equations of magnetohydrodynamics of the convective layer (corresponding physically to (MHD) and integrating them over the closed volume the solar effective temperature) be constant with lat- of the convection zone, we have been able to show itude. For the Sun, this is in line with observations

142 that show no significant dependence of the effective We measured the magnetic field of a sample ofK temperature with latitude. By contrast, if instead the and M dwarfs by analyzing the Zeeman splitting ef- entropy at the outer boundary is fixed (keeping all fect on infrared spectra observed with the Immersion other simulation parameters constant), the outward GRating INfrared Spectrometer (IGRINS). Magnetic conductive flux is allowed to vary with latitude anda field strengths were measured by fitting a double- markedly different rotation profile emerges, namely Lorentzian to Sodium, Calcium, and Titanium lines. one that has cylindrical contours and strong rota- Knowledge of the magnetic field can be used to im- tion gradients confined mainly to low latitudes. We prove stellar interior models and theories on mag- discuss in detail how the outer boundary condition netic field generation. From the initial archive of on the entropy (fixed flux vs. fixed entropy) affects >2500 spectra observed with IGRINS, 1075 were cho- the dynamics responsible for the differential rotation sen for analysis based on the quality of the data and achieved in our simulations. the exclusion of young and old stars that have not yet been calibrated. We determined precise magnetic field measurements for ∼250 objects and upper lim- 319 — Karen Harvey Prize Lecture: its for ∼600 objects. The results of our research give Where Do Solar Eruptions Come us a new understanding of typical magnetic field strengths for low-mass stars and the dependence of From?, Anthony Yeates (Durham these fields on changes to stellar interiors. University) 322.02 — A Universal Spin-Mass Relation for 319.01 — Where Do Solar Eruptions Come From? Brown Dwarfs and Planets Anthony R. Yeates1 Dawn Peterson1; Aleks Scholz2; Keavin Moore3; Ray 4 5 6 1 Durham University (Durham, United Kingdom) Jayawardhana ; Suzanne Aigrain ; Beate Stelzer 1 Space Science Institute (Boulder, Colorado, United States) An oft-quoted idea in solar physics is that coronal 2 Univ. of St Andrews (St Andrews, United Kingdom) mass ejections are, fundamentally, the Sun’s way of 3 McGill University (Montreal, Quebec, Canada) shedding the magnetic helicity that is continually 4 Cornell University (Ithaca, New York, United States) generated by its interior flows. In this talk, I will 5 All Souls College (Oxford, United Kingdom) show how models are helping to give us a handle 6 University Tübingen (Tübingen, Germany) on the build up of magnetic helicity in the corona (the Sun’s lower atmosphere): how much is injected, While brown dwarfs show similarities with stars in where it collects, and how it is ultimately ejected. their early life, their spin evolution is more similar to This endeavour is challenging because it requires us that of planets. We used lightcurves from the K2 mis- to move beyond static (but comfortable) potential- sion to measure new rotation periods for 18 young field extrapolations and develop time-evolving mag- brown dwarfs in the Taurus star-forming region. netic field models for the corona. At the quantita- Our sample spans masses from 0.02 to 0.08 solar tive level, even the definition of magnetic helicity is masses and has been characterized extensively in the non-trivial. The relative magnetic helicity provides past. To search for periods, we utilized three differ- an excellent starting point, but to identify the spatial ent methods (autocorrelation, periodogram, Gaus- distribution of helicity within the corona we need a sian Processes). Our results show the median period finer-grained measure. I will argue that ”field line for brown dwarfs with disks is twice as long as for helicity” is a promising tool for this task, but it is only those without, a signature of rotational braking by beginning to be developed the disk, albeit with small numbers. In addition, we confirmed the presence of a linear increase of the typ- ical rotation period as a function of mass in the sub- 322 — iPoster Session: Stars & stellar regime. The rotational velocities, when calcu- Friends II lated forward to the age of the solar system assum- ing angular momentum conservation, fit the known 322.01 — Measuring the Magnetic Field Strengths spin-mass relation for solar system planets and extra- of K and M Stars solar planetary-mass objects. This spin mass trend holds over six orders of magnitude in mass, includ- 1 1 Maryam Hussaini ; Gregory Mace ing objects from several different formation paths. 1 Astronomy, University of Texas at Austin (Round Rock, Texas, Our result implies that brown dwarfs by and large United States)

143 retain their primordial angular momentum through hot EHB stars might result from He-enhancement (in the first few Myr of their evolution. such clusters) from material enriched by the ejecta of earlier-generation AGB stars. Alternatively, the ex- 322.03 — Stellar Activity of Main Sequence Stars treme mass loss, which might take place in hot subd- warf star progenitors, could be explained through bi- 1 1 4 Alex Larson ; Brendan P. Miller ; Steven H. Saar ; nary interactions. Here, the extreme mass loss would 2 3 5 Elena Gallo ; Jason Wright ; Cedric Hagen be the result of the sdB progenitor experiencing a 1 The College of St. Scholastica (Duluth, Minnesota, United States) period of Roche Lobe Overflow (RLOF). Han et al. 2 University of Michigan (Ann Arbor, Michigan, United States) (2002, 2003) explored such binary formation chan- 3 Pennsylvania State University (Centre County, Pennsylvania, nels for hot subdwarf stars for Z=0.02, presenting a United States) compelling theoretical analysis of three possible bi- 4 Smithsonian Astrophysical Observatory (Cambridge, Mas- nary formation scenarios for sdB stars from either a sachusetts, United States) series of common envelope (CE) phases of mass loss, 5 Oregon State University (Corvallis, Oregon, United States) or stable mass loss due to RLOF, or due to the merger Many main sequence stars have chromospheric ac- of two He WD stars. Their results correlated well tivity levels that vary with time. These can be char- with the finding from Maxted et al. (2001) that most acterized based on their Ca II H and K line core field sdB stars are found in binary systems. In turn, emission. Using data obtained from the California Brown has studied the same binary formation chan- Planet Search we fit a sinusoidal function to a sam- nels, this time for multiple chemical environments ple of 244 stars to test for significant cyclic variabil- having different metallicities (Z=0.0001, 0.001, 0.02, ity. We wrote a python program to analyze obser- 0.03, 0.04, 0.05). The era the Kepler and Gaia sur- vations taken over timescales of up to 17 years to veys has presented ample data to be able to begin to determine optimal sinusoidal parameters, with un- test these binary formation channels, something ex- certainties estimated through a bootstrapping tech- plored in this poster. nique. We also identify some inactive stars with vir- tually no R’HK variability. We find that within our 322.05 — Photometric Observations and Modeling sample the less active cyclic stars tend to have longer of Eclipsing Binaries NSVS 4312042 and NSVS periods. Ongoing work examines the potential im- 2910034 pact of cyclic and flaring stellar activity on known R. Wes Tobin1; Robert C. Berrington2 exoplanets, including those orbiting within the hab- 1 itable zone. Natural Sciences, Indiana University East (Richmond, Indiana, United States) 2 Ball State University (Muncie, Indiana, United States) 322.04 — Hot subdwarf B stars in the age of Kepler and Gaia We present BVR photometric observations and pre- David Brown1 liminary analyses of two eclipsing binary systems: 1 astrophysics, Vatican Observatory (Vatican City, Holy See [Vati- NSVS 4312042 and NSVS 2910034. Systems are mod- can City State]) eled using the PHysics Of Eclipsing BinariEs pro- gram, which utilizes the Wilson-Devinney code to Hot subdwarf B stars are thought to be core-He burn- determine best-fit stellar models. Modeling provides ing stars having masses of approximately 0.5M⊙ , some constraint on the physical parameters of each surrounded by thin hydrogen envelopes with masses system, even without radial velocity measurements. of Menv≤ 0.02M⊙. They are the field equivalents of Preliminary results of NSVS 4312042 indicate that it extreme horizontal branch (EHB) stars in globular appears as a typical contact binary that matches ex- clusters. Although their formation mechanisms re- pectations as a W UMa system. Preliminary results main unknown, it is thought that they form from of NSVS 2910034 indicate that the light curve exhibits progenitors which have experienced a phase of rapid a discernible O’Connell effect. Modeling of NSVS mass loss, typically when they are in the red gi- 2910034 appears to suggest that it may be a semi- ant branch stage of evolution, shortly before igni- detached binary system, which would be inconsis- tion of their helium cores. Single-star progenitor tent with its initial classification as a W UMa system. scenarios of their formation posit that the mass loss Implications and likelihoods are discussed. in EHB progenitors is due either to a high stellar wind and/or a weak binding energy for their en- velopes. Then again, evidence of multiple popula- tions found in globular clusters suggests that such

144 322.06 — A Search for Helium-Core White Dwarfs impurity of neutron star crust and the radius of the in the Globular Cluster 47 Tuc star. ∼100 combinations of possible radii, crust pres- sures, star masses, and maximum possible mass be- Sarah Deveny1; Adrienne Cool1; Craig O. Heinke2; Lil- 6 3 fore black hole collapse were generated by an equa- iana Rivera Sandoval ; Maureen van den Berg ; Jay tion of state (EOS) and were used to arrive at the pre- Anderson4; Phyllis Lugger5; Haldan Cohn5 1 viously mentioned conclusion. Current research fo- San Francisco State University (Danville, California, United cuses on demonstrating a more in-depth relationship States) between the neutron star radius and crustal impurity 2 University of Alberta (Edmonton, Alberta, Canada) 3 by using ∼4000 combinations of generated parame- Harvard University (Cambridge, Massachusetts, United States) ters created by multiple EOSs. 4 Space Telescope Science Institute (Baltimore, Maryland, United States) 322.08 — Machine Learning for Turbulence in 5 Indiana University (Bloomington, Indiana, United States) Supernovae 6 Texas Tech University (Lubbock, Texas, United States) Platon Karpov1,2; Chengkun Huang2; Ghanshyam We report preliminary results of a search for helium- Pilania2; Stan E. Woosley1; Chris Fryer2 core white dwarfs (He WDs) in the globular cluster 1 Astronomy & Astrophysics, UC Santa Cruz (Staten Island, New 47 Tuc. These low-mass white dwarfs are understood York, United States) to form in binary systems in which a star’s evolu- 2 Los Alamos National Laboratory (Los Alamos, New Mexico, tion is interrupted as it climbs the red giant branch. United States) As such, He WDs can provide a window into the binary star populations in globular clusters. Using Turbulence plays a significant role in many different WFC3/UVIS data from the Hubble Space Telescope phenomena, including Core-Collapse Supernovae in two filters, F300X and F390W, we construct a color- (CCSN). Unfortunately, current state-of-the-art sim- magnitude diagram and begin by selecting a subset ulations have to resort to using subgrid models for of the best-measured stars in the cluster. From this turbulence treatment, as direct numerical simula- cleaned diagram we isolate a population of ∼50 can- tions (DNS) are too expensive to run. However, said didate low-mass white dwarfs. Comparing the ra- subgrid models, such as large eddy simulation (LES), dial distribution of these stars to the radial distribu- lack accuracy when compared to DNS results. Re- tions of other populations of known mass in 47 Tuc, cently, there has been a new trend of utilizing Ma- we show that the He WDs are more centrally concen- chine Learning (ML) technique, with impressive pre- trated than can be explained if they are single stars. diction capability for the turbulence closure. We This makes 47 Tuc the third cluster in which a signif- have applied Kernel Ridge Regression to investigate icant population of probable binary stars containing the accuracy and applicability of these algorithms He WDs has been identified. in regards to magnetohydrodynamic (MHD) turbu- lence subgrid modeling. Our future goal is to ready 322.07 — Digging Deeper into the Properties of a and apply our ML methodology within the multi-D Cooling Neutron Star’s Crust MHD CCSN framework to investigate the effects of

1 1 1 accurately-modeled turbulence on the explosion rate Michael Ross ; William Newton ; Lauren Balliet of these events. 1 Physics and Astronomy, Texas A&M University - Commerce (Greenville, Texas, United States)

Low Mass X-ray Binaries are star systems in which a neutron star or a small black hole is paired with a companion star with mass comparable to that of the sun. During accretion, the companion star do- nates matter to the compact object in the system and increases its temperature. When accretion ends, a stage called quiescence, the compact object begins to cool as it moves back toward thermal equilibrium. Properties of various neutron stars’ crusts can be modeled based on how long the stars take to return to thermal equilibrium. Previous research demon- strated an inverse-square relationship between the

145 400 — Plenary Session: From (SCSU), Director of the SCSU Planetarium, and Hon- orary/Adjunct Associate Professor at the University Native Skywatchers to ASTR of Southern Queensland (USQ) in the Centre for As- 101…New Designs for trophysics, Distinguished Lecturer-Archaeological Institute of America (IAI)-Webster Lectureship, and Interdisciplinary, an American Astronomical Society (AAS) Shapley Multidisciplinary, and Lecturer. Annette is mixed-race Lakota and her com- munities are Ojibwe and D/Lakota. Transdisciplinary Engaged Learning Now, Annette Lee (St. 400.02 — Cahokia Mounds: America’s First City Cloud University) and Bill William Iseminger1 Iseminger (Cahokia Mounds 1 Cahokia Mounds State Historic Site (Collinsville, Illinois, United States) Historic Site) Cahokia Mounds was the largest prehistoric In- 400.01 — From Native Skywatchers to ASTR 101 dian community in America north of Mexico and … New Designs for Interdisciplinary, at its height covered six square miles, included 120 Multidisciplinary, and Transdisciplinary Engaged earthen mounds, and a population estimated to have Learning Now been 10-20,000. Built by the Mississippian culture, it flourished from about AD 1000-1350. The pre- 1,2 Annette S. Lee sentation will include discussions of the culture and 1 Physics and Astronomy, St. Cloud State University (St. Cloud, the major site features, including the Woodhenge Minnesota, United States) sun calendars, the defensive Palisade wall, the ritual 2 University of Southern Queensland (Toowoomba, Queensland, burials of Mound 72, the Grand Plaza, and 100-foot- Australia) high Monks Mound, the largest prehistoric earth- work in the Americas. It was also the center of a “Learn to see from one eye with the best in Indigenous major prehistoric urban complex known as Greater knowledges, and from the other eye with the best in West- Cahokia that included the mound complexes in St. ern knowledge…and learn to use both these eyes together Louis and East St. Louis, smaller mound sites, and for the benefit of all… the gift of multiple perspectives.” — numerous moundless hamlets and farmsteads. Elder Albert Marshall from the Mi’kmaq Nation Designed by Lee, the Native Skywatchers initiative seeks to remember and revitalize indigenous star 401 — iPoster Plus XI: (SPD), and earth knowledge, promoting the native voice as the lead voice. The overarching goal of Native Sky- Magnetic Fields watchers is to communicate the knowledge that in- digenous people traditionally practiced a sustainable 401.01 — Long-Term Prediction of Solar Activity way of living and sustainable engineering through a Using Magnetogram Data and Ensemble Kalman living and participatory relationship with the above Filter and below, sky and earth. We aim to improve cur- Irina Kitiashvili1; Alexander G. Kosovichev2 rent inequities in education for native young peo- 1 NASA Ames Research Center (Mountain View, California, United ple, to inspire increased cultural pride, and promote States) community wellness. We hope to inspire all people 2 New Jersey Institute of Technology (Newark, New Jersey, United to have a rekindling or deepening sense of awe and States) personal relationship to the cosmos. Presented here will be strategies and best practices for effective and Solar activity predictions using the data assimila- inclusive widening participation in science through tion approach have demonstrated great potential to astronomy. Of particular emphasis will be the con- build reliable long-term forecasts of solar activity. nection between indigenous worldviews, narrative, In particular, it has been shown that the Ensemble and the visual language, and how this informs the Kalman Filter (EnKF) method applied to a non-linear teaching and strategies in large lecture introductory dynamo model is capable of predicting solar activ- astronomy college courses. ity up to one sunspot cycle ahead in time, as well Currently Annette is an Associate Professor of As- as estimating the properties of the next cycle a few tronomy & Physics at St. Cloud State University years before it begins. These developments assume

146 an empirical relationship between the mean toroidal patches of enhanced radial field are compared with magnetic field flux and the sunspot number. Esti- certain types of solar activity such as coronal jets. mated from the sunspot number series, variations of We emphasize the limitation of the existing data for the toroidal field have been used to assimilate the studying polar field. data into the Parker-Kleeorin-Ruzmakin (PKR) dy- namo model by applying the EnKF method. The dy- namo model describes the evolution of the toroidal 402 — Solar Physics Division and poloidal components of the magnetic field and Meeting (SPD), Magnetic Fields the magnetic helicity. Full-disk magnetograms pro- vide more accurate and complete input data by con- 402.01 — Evolution of Flows around Emerging straining both the toroidal and poloidal global field Active Regions components, but these data are available only for the last four solar cycles. In this presentation, using Nils Gottschling1; Hannah Schunker1; Aaron C. Birch1; the available magnetogram data, we discuss devel- Laurent Gizon1 opment of the methodology and forecast quality cri- 1 Solar and Stellar Interiors, Max Planck Institute for Solar System teria (including forecast uncertainties and sources of Research (Goettingen, Lower Saxony, Germany) errors). We demonstrate the influence of limited time series observations on the accuracy of solar activity Inflows associated with established active regions predictions. We present EnKF predictions of the up- have been measured with velocities of about 30 m/s coming Solar Cycle 25 based on both the sunspot and extending up to 10° from the active regions, but number series and observed magnetic fields and dis- have so far been included in surface flux transport cuss the uncertainties and potential of the data as- models only in a simple form. How these flows de- similation approach. The research is funded by the velop as active regions emerge has not yet been stud- NSF SHINE program AGS-1622341. ied. We measure the flows surrounding 182 emerg- ing active regions observed by the SDO/HMI instru- 401.02 — (withdrawn) ment using local correlation tracking of the granula- tion as they evolve from seven days before to seven This abstract was withdrawn. days after emergence. We find flows converging to- wards the trailing polarity at the time when magnetic 401.03 — Polar magnetic field in solar cycle 24 flux first emerges. Three days later, extended inflows form towards the center of the active region predom- 1 Nariaki Nitta inantly in the north-south direction, together with 1 Lockheed Martin, ATC (Palo Alto, California, United States) outflows at the leading polarity, due to moat flows around sunspots. The flows have velocities of 20to Coronal holes often sit in Sun’s polar regions, and 30 m/s and increase in extent from about 2° to about they are believed to be responsible for the fast solar 7°. At later times, the flows resemble those from pre- wind. The magnetic field therein is open to the he- vious studies of established active regions. These re- liosphere. It is possible that such field may emanate sults will help constrain models of the surface evolu- from small patches with enhanced field strength, tion of magnetic fields. which were first revealed in data from the Spectropo- larimeter (SP) of the Hinode Solar Optical Telescope. 402.02 — Measuring and Characterizing the It has recently been shown that very similar patches Importance of Magnetic Flux Cancellation in Solar can be found in vector magnetograms from the He- Active Regions during their Emergence Phase lioseismic and Magnetic Imager (HMI) on the Solar Dynamics Observatory (SDO), even though SP has Georgios Chintzoglou1; Mark Cheung1 better spatial resolution and vector magnetography. 1 Lockheed Martin Solar and Astrophysics Lab (Palo Alto, Califor- An advantage of SDO/HMI is constant availability of nia, United States) full-disk vector data. This allows us to make movies of radial field in polar regions with varying cadences, Active Regions (ARs) in their emergence phase are which can be used to study the dynamical evolution known to be more flare productive and eruptive than of the patchy magnetic field regions in high latitudes, ARs in their decay phase. For decaying ARs, the such as poleward of 60 degrees, generally difficult flaring and eruptive activity is thought to be acon- to observe from an ecliptic vantage point. We dis- sequence of the formation of magnetic flux ropes cuss the general distribution of magnetic field in po- through photospheric magnetic flux cancellation, of- lar regions over solar cycle 24 using such movies. The ten occurring at the internal polarity inversion line

147 (PIL) of the AR. Typically, during the AR decay 3 Space Science Laboratory, University of California Berkeley phase, flux cancellation manifests itself by a clear de- (Berkeley, California, United States) cay of the total unsigned magnetic flux, sometimes preceding and even accompanying the flaring and The advent of routine photospheric vector magne- eruptive activity. In emerging ARs, however, no can- tograms now allows for realistic estimate of active cellation can be seen in the total unsigned magnetic region (AR) energy and helicity flux. Such esti- flux owing to sustained flux emergence. In this work mate requires information of the surface velocity we focus on complex emerging ARs composed of field. Here, we calculate the energy and helicity flux multiple bipoles. Due to the compact clustering of for AR 12673 where significant Doppler flows (Vl) the different bipoles within such complex multipolar were observed along the magnetic polarity inversion ARs, collision and shearing between opposite non- line. Results based on the DAVE4VM velocity esti- conjugated polarities drives rapid photospheric can- mate (without Vl information) and the CGEM elec- cellation. This mechanism is called collisional shear- tric field inversion (with Vl) algorithms differ signif- ing. In Chintzoglou et al (2019), it was demonstrated icantly, mainly due to the additional constraint from that collisional shearing occurred in two emerging Vl. We argue that Dopper velocity needs to be in- flare and CME productive ARs (NOAA AR11158 and cluded for realistic flux estimate. We describe an up- AR12017) and a significant amount of cancelled flux dated DAVE4VMWDV velocity estimate algorithm was measured by applying the conjugate flux deficit that incorporates such contribution. method (Chintzoglou et al 2019). Here, we employ a new methodology based on a novel electric field in- 402.05 — Multi-wavelength Multi-height Study of version method and we calculate the time evolution Super Strong Surface and Coronal Magnetic of magnetic flux through Faraday’s law at the inter- Fields in Active Region 12673 nal PIL of emerging ARs. We compare this method- Haimin Wang2; Bin Chen1; Ju Jing2; Sijie Yu1; Chang ology with the conjugate flux deficit method on mag- 2 2 2 netogram series of synthetic and observed emerging Liu ; Vasyl B. Yurchyshyn ; Kwangsu Ahn ; Takenori Okamoto3; Shin Toriumi3; Wenda Cao2; Dale E. Gary1 ARs and discuss our results in relation to flare and 1 eruptive activity. NJIT (Newark, New Jersey, United States) 2 Big Bear Solar Observatory (Big Bear Lake, California, United States) 402.03 — On Evolution of Magnetic Helicity in 3 NAOJ (Mitaka, Japan) Solar Bipole Active Regions Yang Liu1 Using the joint observations of Goode Solar tele- 1 Stanford University (Palo Alto, California, United States) scope (GST), Expanded Owens Valley Solar Array (EOVSA), Solar Dynamics Observatory (SDO) and Using SDO/HMI vector magnetic field data, we Hinode, we study the Solar Active Region (AR) 12673 study magnetic helicity evolution in bipole active re- in September 2017, which is the most flare produc- gions. We compute helicity flux through the photo- tive AR in the solar cycle 24. GST observations show sphere for a sample of emerging active regions with the strong photospheric magnetic fields (nearly 6000 bipole magnetic configuration. We then explore rela- G) in polarity inversion line (PIL) and apparent pho- tionship between the accumulated helicity in the ac- tospheric twist. Consistent upward flows are also ob- tive regions and the total magnetic flux. A relation- served in Dopplergrams of Hinode, HMI and GST ship between helicity and magentic flux is found ina at the center part of that section of PIL, while the subgroup of the active regions, suggesting a unique down flows are observed in two ends, indicating that property of magnetic twist in these active regions. the structure was rising from subsurface. Combining We discuss implication of this relationship here. Non-Linear Force Free Extrapolation and EOVSA mi- crowave imaging spectroscopy, we also look into the 402.04 — Contribution of Doppler Velocity to coronal structure of magnetic fields in this unusual Active Region Energy and Helicity Flux Estimate AR, including the evolution before and after the X9.3 flare on September 6, 2017. Coronal fields between Xudong Sun1; Peter W. Schuck2; George H. Fisher3 1000 and 2000 gauss are found above the flaring PIL 1 Institute for Astronomy, University of Hawaii (Pukalani, Hawaii, at the height range between 8 and 4Mm, outlining United States) the structure of a fluxrope or sheared arcade. 2 NASA Goddard Space Flight Center (Washington, District of Columbia, United States)

148 403 — Gravitational Waves & consistently calculated crust model and a set of neu- tron skin and nuclear giant resonance predictions, Instrumentation: Space Missions allowing consistent propagation of constraints be- tween the nuclear and astrophysical domains. 403.01 — Searches in Advanced LIGO and Advanced Virgo data for continuous gravitational 403.03 — Measuring the tidal deformability of waves GW170817’s component stars using consistent Keith Riles1 chiral-EFT equations of state 1 University of Michigan (Ann Arbor, Michigan, United States) Collin Capano1; Stephanie Brown1; Ingo Tews2; Duncan 3 1 4,5 The LIGO Scientific Collaboration and Virgo Collab- Brown ; Badri Krishnan ; Sanjay Reddy 1 oration have carried out joint searches in Advanced Albert Einsten Institute, Hannover (Hannover, Niedersachsen, LIGO and Advanced Virgo data (observing runs Germany) 2 O1 and O2) for periodic continuous gravitational Theoretical Division, Los Alamos National Laboratory (Los waves. These analyses range from targeted searches Alamos, New Mexico, United States) 3 for gravitational-wave signals from known pulsars, Syracuse University (Syracuse, New York, United States) 4 for which ephemerides from radio, X-ray or gamma- Institute for Nuclear Theory, University of Washington (Seattle, ray observations are used in precise templates, to all- Washington, United States) 5 sky searches for unknown neutron stars, including JINA-CEE, Michigan State University (East Lansing, Michigan, stars in binary systems. Between these extremes lie United States) directed searches for known stars of unknown spin frequency or for new unknown sources at specific lo- GW170817 provided the unprecedented opportunity cations, such as near the galactic center. Recent and to constrain the equation of state (EOS) of matter ongoing searches of each type will be summarized, at super-nuclear densities using gravitational waves. along with prospects for future searches using more This has been accomplished via Bayesian inference sensitive data from the ongoing O3 observing run of the mass and tidal deformation of the component and from future runs. objects. Previous studies assumed that the EOS of the components of GW170817 were either exactly the same, or completely uncorrelated. Neither of these 403.02 — Linking neutron star observations and assumptions is expected to be entirely correct if the nuclear observables consistently component objects are neutron stars. Chiral effective William Newton1 field theory (EFT) provides a framework for quanti- 1 Texas AandM University-Commerce (Dallas, Texas, United fying the uncertainty in a neutron star’s EOS due to States) two- and three-nucleon interactions. In this study, we consider generic equations of state from chiral Using a new suite of equations of state parameter- EFT when using Bayesian inference to measure the ized entirely by neutron star and nuclear observ- tidal deformability of the components of GW170817. ables, we explore consistently the correlations be- This can allow us to constrain the allowed EFTs from tween neutron star crust and core properties, neu- gravitational-wave observations. tron skins and other nuclear observables. The equa- tions of state are based on an extended Skyrme en- 403.04 — NASA Astrophysics CubeSats and ergy density functional up to one and a half times SmallSats saturation density, and on polytropes at higher den- sities. Each equation of state is characterized by Michael R. Garcia1; Nasser Barghouty1; Stefan Immler1; 5 parameters: the first three symmetry energy pa- William B. Latter1 rameters in its density expansion about saturation 1 Astrophysics, NASA HQ (Washington, District of Columbia, density, the moment of inertia of 1.337 solar mass United States) neutron star, and the neutron star maximum mass. The three symmetry energy degrees of freedom are The NASA Astrophysics Division is currently fund- varied to systematically cover the whole parameter ing five science CubeSats which are in various stages space allowed by microscopic calculations of pure of operation or construction, and also nine studies neutron matter, and the remaining parameters uni- of astrophysics science SmallSats. I review the sta- formly span the range of values consistent with tus of these, the funding opportunities, and possible causality and the existence of a 2.0 solar mass neu- path(s) forward. tron star. Each equation of state comes with its own

149 403.05 — Placeholder: Abstract Moved 402.05 ability to return the science without disruption. In- creasing the degree of autonomy is enhancing to all 403.06 — Updated Standard Evaluation of space- and ground-based observatories by defining exoplanet Yield for the LUVOIR and HabEx resilient operations where science can continue de- Concept Studies spite anomalies, and increasing observing capability Rhonda Morgan1; Bertrand Mennesson1; Dmitry while reducing costs. Savransky2; Eric E. Mamajek1; Stuart Shaklan1; Karl An autonomous observing system can respond R. Stapelfeldt1; Michael Turmon1; Walker Dula1 to failures by exploring different strategies to retry 1 Jet Propulsion Laboratory (Pasadena, California, United States) or attempt corrective measures to resume nominal 2 Cornell University (Ithaca, New York, United States) operation. An autonomous framework defines a distinction between system-level and function-level The HabEx and LUVOIR concepts aim to directly control that is generic to the mission system; thus, image and spectrally characterize potentially habit- patterns of behavior on one mission can be utilized able exoplanets. Using EXOSIMS, realistic mission on other missions to reduce development, testing, observing constraints, and dynamically responsive and operational costs. scheduling, we simulate the exoplanet detection and System-level autonomy enables new architectures. characterizations over Monte Carlo realizations of Here, the planning/schedule approach for a sin- synthetic planets around nearby stars. We use identi- gle spacecraft can be generalized to support multi- cal astrophysical inputs and the observing scenarios ple spacecraft using multi-agent autonomy. Com- of each concept to evaluate a common comparison plex, interferometric missions – like LISA – are en- of the detection and spectral characterization yields abled. Similarly transient event missions, like those of HabEx and LUVOIR. HabEx is evaluated for the observing multi-messenger signals, can be designed 4m hybrid starshade and coronagraph architecture, at lower cost as transient response no longer needs to the 4m coronagraph only architecture, and the 3.2 be custom designed for that given mission, but is de- m starshade only architecture. LUVOIR is evaluated signed as an extension to existing autonomous plan- for the 15 m on-axis and 9 m off-axis architectures. ning/execution capabilities. System-level autonomy The scenarios are scheduled to respond dynamically can be deployed on ground-based observatories to to the number of detections/no-detections of a tar- respond dynamically to sky conditions to execute al- get and success of characterization as well as the op- ternate observations when scheduled observations timal slews for the starshade. Yield analysis shows are not possible. that both concepts can directly image and spectrally characterize earth-like planets in the Habitable zone 403.08 — (withdrawn) and that each concept has complementary strengths. This abstract was withdrawn. 403.07 — Enhanced and Enabled Astrophysical Observations with System-Level Autonomy 404 — Plenary Lecture: The Apollo Rashied Amini1 Lunar Exploration Program: 1 NASA JPL (Pasadena, California, United States) Scientific Impact and the Road A system-level autonomy framework enables a com- plex system to accomplish stated goals while observ- Ahead, James Head (Brown ing and reacting to changes within the system and its University) operating environment without traditional human intervention. As witnessed in automotive and avia- 404.01 — The Apollo Lunar Exploration Program: tion sectors, system-level autonomy has realized ca- Scientific Impact and the Road Ahead pabilities only previously imagined. The impact of 1 these capabilities on our ability to observe the uni- James W. Head 1 verse will be just as revolutionary. Brown Univ. (Providence, Rhode Island, United States) The missions and systems currently under study for the Astro2020 Decadal are larger in size and more Half a century ago, the Apollo lunar exploration mis- complex than past missions, with larger platforms, sions began the transformation of the Moon, terres- actuated optics, multiple flight systems, and com- trial planets and outer planet satellites, from objects plicated focal planes. With new complexity comes of astronomical study to objects of geologic explo- new threats to nominal operations and a mission’s ration and characterization. The Apollo missions re-

150 solved fundamental questions about the Moon (Ori- gin of the Moon and its craters, the age and origin of the maria, the formation of basins; Did the Moon form hot or cold?). It also provided a fundamen- tal framework and paradigm for understanding the history and evolution of the terrestrial planets, in- cluding Earth. What have we learned about plan- etary formation and evolution in the ensuing five decades from this Moon-based comparative plane- tology? Ejecta from a large Mars-sized projectile im- pacting into early Earth appears to have formed the Moon. Impact cratering plays a fundamental role in initial impact heating and melting to create a molten magma ocean whose thermal and chemical evolu- tion dictates much of subsequent history. Planetary internal heating, melting and extrusion of molten rock (lava) to the surface supplies additional volatiles to the primordial atmospheres and resurfaces signif- icant areas. Earth loses heat through plate tectonics, but smaller bodies lose heat primarily by conduction and rapidly become “one-plate planets”. Planets lose atmospheres as a function of time and Mars is a labo- ratory for this change, perhaps evolving from warm and wet to today’s sub-freezing desert. The current position of planets relative to their stars is not nec- essarily where they started out. Abundant plane- tary environments have the ingredients for life, but life has thus far only been detected on Earth. As usual, astronomers are leading the way to the fu- ture, with the discovery of many dozens of exoplane- tary systems and thousands of exoplanets. Today as- tronomers and planetary scientists are teaming up to tackle fundamental questions in comparative plane- tary systems: How can we use our knowledge about our Solar System and the characteristics and histo- ries of its planets and satellites to interpret the na- ture of exoplanets? Where does the Solar System fit in the menagerie of exoplanetary systems? Is our So- lar System typical or anomalous?

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