Kepler & K2 Science Conference V Program
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Arxiv:2007.10995V1
Draft version July 23, 2020 Typeset using LATEX twocolumn style in AASTeX63 Transits of Known Planets Orbiting a Naked-Eye Star Stephen R. Kane,1 Selc¸uk Yalc¸ınkaya,2 Hugh P. Osborn,3,4,5 Paul A. Dalba,1, ∗ Louise D. Nielsen,6 Andrew Vanderburg,7, † Teo Mocnikˇ ,1 Natalie R. Hinkel,8 Colby Ostberg,1 Ekrem Murat Esmer,9 Stephane´ Udry,6 Tara Fetherolf,1 Ozg¨ ur¨ Bas¸turk¨ ,9 George R. Ricker,4 Roland Vanderspek,4 David W. Latham,10 Sara Seager,4,11,12 Joshua N. Winn,13 Jon M. Jenkins,14 Romain Allart,6 Jeremy Bailey,15 Jacob L. Bean,16 Francois Bouchy,6 R. Paul Butler,17 Tiago L. Campante,18,19 Brad D. Carter,20 Tansu Daylan,4, ‡ Magali Deleuil,3 Rodrigo F. Diaz,21 Xavier Dumusque,6 David Ehrenreich,6 Jonathan Horner,20 Andrew W. Howard,22 Howard Isaacson,23,20 Hugh R.A. Jones,24 Martti H. Kristiansen,25,26 Christophe Lovis,6 Geoffrey W. Marcy,23 Maxime Marmier,6 Simon J. O’Toole,27,28 Francesco Pepe,6 Darin Ragozzine,29 Damien Segransan,´ 6 C.G. Tinney,30 Margaret C. Turnbull,31 Robert A. Wittenmyer,20 Duncan J. Wright,20 and Jason T. Wright32 1Department of Earth and Planetary Sciences, University of California, Riverside, CA 92521, USA 2Ankara University, Graduate School of Natural and Applied Sciences, Department of Astronomy and Space Sciences, Tandogan, TR-06100, Turkey 3Aix-Marseille Universit, CNRS, CNES, Laboratoire d’Astrophysique de Marseille, France 4Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 5NCCR/PlanetS, Centre for Space & Habitability, University of Bern, Bern, Switzerland 6Observatoire de Gen`eve, Universit´ede Gen`eve, 51 ch. -
Abstracts Connecting to the Boston University Network
20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes. -
Jason A. Dittmann 51 Pegasi B Postdoctoral Fellow
Jason A. Dittmann 51 Pegasi b Postdoctoral Fellow Contact Massachusetts Institute of Technology MIT Kavli Institute: 37-438f 617-258-5928 (office) 70 Vassar St. 520-820-0928 (cell) Cambridge, MA 02139 [email protected] Education Harvard University, Cambridge, MA PhD, Astronomy and Astrophysics, May 2016 Advisor: David Charbonneau, PhD • University of Arizona, Tucson, AZ BS, Astronomy, Physics, May 2010 Advisor: Laird Close, PhD • Recent 51 Pegasi b Postdoctoral Fellow July 2017 – Present Research Earth and Planetary Science Department, MIT Positions Faculty Contact: Sara Seager Postdoctoral Researcher Feb 2017 – June 2017 Kavli Institute, MIT Supervisor: Sarah Ballard Postdoctoral Researcher July 2016 – Jan 2017 Center for Astrophysics, Harvard University Supervisor: David Charbonneau Research Assistant Sep 2010 – May 2016 Center for Astrophysics, Harvard University Advisors: David Charbonneau Publication 16 first and second authored publications Summary 22 additional co-authored publications 1 first-authored publication in Nature 1 co-authored publication in Nature Selected 51 Pegasi b Postdoctoral Fellowship 2017 – Present Awards and Pierce Fellowship 2010 – 2013 Honors Certificate of Distinction in Teaching 2012 Best Project Award, Physics Ugrd. Research Symp. 2009 Best Undergraduate Research (Steward Observatory) 2009 – 2010 Grants Principal Investigator, Hubble Space Telescope 2017, 10 orbits Awarded “Initial Reconaissance of a Transiting Rocky (maximum award) Planet in a Nearby M-Dwarf’s Habitable Zone” Principal Investigator, -
Exoplanet Exploration Collaboration Initiative TP Exoplanets Final Report
EXO Exoplanet Exploration Collaboration Initiative TP Exoplanets Final Report Ca Ca Ca H Ca Fe Fe Fe H Fe Mg Fe Na O2 H O2 The cover shows the transit of an Earth like planet passing in front of a Sun like star. When a planet transits its star in this way, it is possible to see through its thin layer of atmosphere and measure its spectrum. The lines at the bottom of the page show the absorption spectrum of the Earth in front of the Sun, the signature of life as we know it. Seeing our Earth as just one possibly habitable planet among many billions fundamentally changes the perception of our place among the stars. "The 2014 Space Studies Program of the International Space University was hosted by the École de technologie supérieure (ÉTS) and the École des Hautes études commerciales (HEC), Montréal, Québec, Canada." While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content. Electronic copies of the Final Report and the Executive Summary can be downloaded from the ISU Library website at http://isulibrary.isunet.edu/ International Space University Strasbourg Central Campus Parc d’Innovation 1 rue Jean-Dominique Cassini 67400 Illkirch-Graffenstaden Tel +33 (0)3 88 65 54 30 Fax +33 (0)3 88 65 54 47 e-mail: [email protected] website: www.isunet.edu France Unless otherwise credited, figures and images were created by TP Exoplanets. Exoplanets Final Report Page i ACKNOWLEDGEMENTS The International Space University Summer Session Program 2014 and the work on the -
Arxiv:2001.10147V1
Magnetic fields in isolated and interacting white dwarfs Lilia Ferrario1 and Dayal Wickramasinghe2 Mathematical Sciences Institute, The Australian National University, Canberra, ACT 2601, Australia Adela Kawka3 International Centre for Radio Astronomy Research, Curtin University, Perth, WA 6102, Australia Abstract The magnetic white dwarfs (MWDs) are found either isolated or in inter- acting binaries. The isolated MWDs divide into two groups: a high field group (105 − 109 G) comprising some 13 ± 4% of all white dwarfs (WDs), and a low field group (B < 105 G) whose incidence is currently under investigation. The situation may be similar in magnetic binaries because the bright accretion discs in low field systems hide the photosphere of their WDs thus preventing the study of their magnetic fields’ strength and structure. Considerable research has been devoted to the vexed question on the origin of magnetic fields. One hypothesis is that WD magnetic fields are of fossil origin, that is, their progenitors are the magnetic main-sequence Ap/Bp stars and magnetic flux is conserved during their evolution. The other hypothesis is that magnetic fields arise from binary interaction, through differential rotation, during common envelope evolution. If the two stars merge the end product is a single high-field MWD. If close binaries survive and the primary develops a strong field, they may later evolve into the arXiv:2001.10147v1 [astro-ph.SR] 28 Jan 2020 magnetic cataclysmic variables (MCVs). The recently discovered population of hot, carbon-rich WDs exhibiting an incidence of magnetism of up to about 70% and a variability from a few minutes to a couple of days may support the [email protected] [email protected] [email protected] Preprint submitted to Journal of LATEX Templates January 29, 2020 merging binary hypothesis. -
PLANETARY CANDIDATES OBSERVED by Kepler. VIII. a FULLY AUTOMATED CATALOG with MEASURED COMPLETENESS and RELIABILITY BASED on DATA RELEASE 25
Draft version October 13, 2017 Typeset using LATEX twocolumn style in AASTeX61 PLANETARY CANDIDATES OBSERVED BY Kepler. VIII. A FULLY AUTOMATED CATALOG WITH MEASURED COMPLETENESS AND RELIABILITY BASED ON DATA RELEASE 25 Susan E. Thompson,1, 2, 3, ∗ Jeffrey L. Coughlin,2, 1 Kelsey Hoffman,1 Fergal Mullally,1, 2, 4 Jessie L. Christiansen,5 Christopher J. Burke,2, 1, 6 Steve Bryson,2 Natalie Batalha,2 Michael R. Haas,2, y Joseph Catanzarite,1, 2 Jason F. Rowe,7 Geert Barentsen,8 Douglas A. Caldwell,1, 2 Bruce D. Clarke,1, 2 Jon M. Jenkins,2 Jie Li,1 David W. Latham,9 Jack J. Lissauer,2 Savita Mathur,10 Robert L. Morris,1, 2 Shawn E. Seader,11 Jeffrey C. Smith,1, 2 Todd C. Klaus,2 Joseph D. Twicken,1, 2 Jeffrey E. Van Cleve,1 Bill Wohler,1, 2 Rachel Akeson,5 David R. Ciardi,5 William D. Cochran,12 Christopher E. Henze,2 Steve B. Howell,2 Daniel Huber,13, 14, 1, 15 Andrej Prša,16 Solange V. Ramírez,5 Timothy D. Morton,17 Thomas Barclay,18 Jennifer R. Campbell,2, 19 William J. Chaplin,20, 15 David Charbonneau,9 Jørgen Christensen-Dalsgaard,15 Jessie L. Dotson,2 Laurance Doyle,21, 1 Edward W. Dunham,22 Andrea K. Dupree,9 Eric B. Ford,23, 24, 25, 26 John C. Geary,9 Forrest R. Girouard,27, 2 Howard Isaacson,28 Hans Kjeldsen,15 Elisa V. Quintana,18 Darin Ragozzine,29 Avi Shporer,30 Victor Silva Aguirre,15 Jason H. Steffen,31 Martin Still,8 Peter Tenenbaum,1, 2 William F. -
Water Worlds Cannot Composition of Planets Ranging from 2 to 4 Earth Radii (R⊕) Still Be Made Based on the Mass–Radius Relationship Alone Or the – Remains
Growth model interpretation of planet size distribution Li Zenga,b,1, Stein B. Jacobsena, Dimitar D. Sasselovb, Michail I. Petaeva,b, Andrew Vanderburgc, Mercedes Lopez-Moralesb, Juan Perez-Mercadera, Thomas R. Mattssond, Gongjie Lie, Matthew Z. Heisingb, Aldo S. Bonomof, Mario Damassof, Travis A. Bergerg, Hao Caoa, Amit Levib, and Robin D. Wordswortha aDepartment of Earth and Planetary Sciences, Harvard University, Cambridge, MA 02138; bCenter for Astrophysics j Harvard & Smithsonian, Department of Astronomy, Harvard University, MA 02138; cDepartment of Astronomy, The University of Texas at Austin, Austin, TX 78712; dHigh Energy Density Physics Theory Department, Sandia National Laboratories, Albuquerque, NM 87185; eSchool of Physics, Georgia Institute of Technology, Atlanta, GA 30313; fIstituto Nazionale di Astrofisica–Osservatorio Astrofisico di Torino, 10025 Pino Torinese, Italy; and gInstitute for Astronomy, University of Hawaii, Honolulu, HI 96822 Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved March 21, 2019 (received for review July 26, 2018) The radii and orbital periods of 4,000+ confirmed/candidate exo- be distributed log-uniform, that is, flat in semimajor axis a or planets have been precisely measured by the Kepler mission. The orbital period P, beyond ∼10d(figure7ofref.12).Suchorbit radii show a bimodal distribution, with two peaks corresponding distributions of both populations challenge the photoevaporation to smaller planets (likely rocky) and larger intermediate-size plan- scenario as the cause of the gap because it strongly depends on the ets, respectively. While only the masses of the planets orbiting the orbital distance. If the gap is caused by photoevaporation, then an brightest stars can be determined by ground-based spectroscopic anticorrelation in their orbital distributions is expected (13). -
A Spectroscopic Analysis of the California-Kepler Survey Sample: I
Draft version March 4, 2019 Typeset using LATEX modern style in AASTeX61 A SPECTROSCOPIC ANALYSIS OF THE CALIFORNIA-KEP LER SURVEY SAMPLE: I. STELLAR PARAMETERS, PLANETARY RADII AND A SLOPE IN THE RADIUS GAP Cintia F. Martinez,1 Katia Cunha,1, 2 Luan Ghezzi,1 and Verne V. Smith3 1Observat´orioNacional, Rua General Jos´eCristino, 77, 20921-400 S~aoCrist´ov~ao,Rio de Janeiro, RJ, Brazil 2Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721, USA 3National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA (Received October, 2018; Revised February, 2019) Submitted to ApJ ABSTRACT We present results from a quantitative spectroscopic analysis conducted on archival Keck/HIRES high-resolution spectra from the California-Kepler Survey (CKS) sam- ple of transiting planetary host stars identified from the Kepler mission. The spectro- scopic analysis was based on a carefully selected set of Fe I and Fe II lines, resulting in precise values for the stellar parameters of effective temperature (Teff ) and surface gravity (log g). Combining the stellar parameters with Gaia DR2 parallaxes and precise distances, we derived both stellar and planetary radii for our sample, with a median internal uncertainty of 2.8% in the stellar radii and 3.7% in the planetary radii. An investigation into the distribution of planetary radii confirmed the bimodal nature of this distribution for the small radius planets found in previous studies, with peaks at: ∼1.47 ± 0.05 R⊕ and ∼2.72 ± 0.10 R⊕, with a gap at ∼ 1.9R⊕. Previous studies that modeled planetary formation that is dominated by photo-evaporation arXiv:1903.00174v1 [astro-ph.EP] 1 Mar 2019 predicted this bimodal radii distribution and the presence of a radius gap, or photo- evaporation valley. -
Characterization of Low-Mass K2 Planet Hosts Using Near-Infrared Spectroscopy
Downloaded from orbit.dtu.dk on: Sep 27, 2021 Characterization of Low-mass K2 Planet Hosts Using Near-infrared Spectroscopy Martínez, Romy Rodríguez; Ballard, Sarah; Mayo, Andrew; Vanderburg, Andrew; Montet, Benjamin T.; Christiansen, Jessie L. Published in: Astrophysical Journal Link to article, DOI: 10.3847/1538-3881/ab3347 Publication date: 2019 Document Version Publisher's PDF, also known as Version of record Link back to DTU Orbit Citation (APA): Martínez, R. R., Ballard, S., Mayo, A., Vanderburg, A., Montet, B. T., & Christiansen, J. L. (2019). Characterization of Low-mass K2 Planet Hosts Using Near-infrared Spectroscopy. Astrophysical Journal, 158(4), [135]. https://doi.org/10.3847/1538-3881/ab3347 General rights Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. Users may download and print one copy of any publication from the public portal for the purpose of private study or research. You may not further distribute the material or use it for any profit-making activity or commercial gain You may freely distribute the URL identifying the publication in the public portal If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. The Astronomical Journal, 158:135 (14pp), 2019 October https://doi.org/10.3847/1538-3881/ab3347 © 2019. The American Astronomical Society. All rights reserved. Characterization of Low-mass K2 Planet Hosts Using Near-infrared Spectroscopy Romy Rodríguez Martínez1, Sarah Ballard2,9, Andrew Mayo3,4,5,10,11 , Andrew Vanderburg6,12 , Benjamin T. -
2020 Science Gap List
ExEP Science Gap List, Rev C JPL D: 1717112 Release Date: January 1, 2020 Page 1 of 21 Approved by: Dr. Gary Blackwood Date Program Manager, Exoplanet Exploration Program Office NASA/Jet Propulsion Laboratory Dr. Douglas Hudgins Date Program Scientist Exoplanet Exploration Program Science Mission Directorate NASA Headquarters EXOPLANET EXPLORATION PROGRAM Science Gap List 2020 Karl Stapelfeldt, Program Chief Scientist Eric Mamajek, Deputy Program Chief Scientist Exoplanet Exploration Program JPL CL#20-1234 CL#20-1234 JPL Document No: 1717112 ExEP Science Gap List, Rev C JPL D: 1717112 Release Date: January 1, 2020 Page 2 of 21 Cover Art Credit: NASA/JPL-Caltech. Artist conception of the K2-138 exoplanetary system, the first multi-planet system ever discovered by citizen scientists1. K2-138 is an orangish (K1) main sequence star about 200 parsecs away, with five known planets all between the size of Earth and Neptune orbiting in a very compact architecture. The planet’s orbits form an unbroken chain of 3:2 resonances, with orbital periods ranging from 2.3 and 12.8 days, orbiting the star between 0.03 and 0.10 AU. The limb of the hot sub-Neptunian world K2-138 f looms in the foreground at the bottom, with close neighbor K2-138 e visible (center) and the innermost planet K2-138 b transiting its star. The discovery study of the K2-138 system was led by Jessie Christiansen and collaborators (2018, Astronomical Journal, Volume 155, article 57). This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. -
Giant Planets Transiting Giant Stars a DISSERTATION SUBMITTED TO
Giant Planets Transiting Giant Stars A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI`I AT MANOA¯ IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN ASTRONOMY August 2019 By Samuel Kai Grunblatt Dissertation Committee: Daniel Huber, Chairperson Eric J. Gaidos Andrew W. Howard Christoph J. Baranec Rolf-Peter Kudritzki Jonathan P. Williams c Copyright 2019 by Samuel K. Grunblatt All Rights Reserved ii To I. Piehler, H. Grunblatt, and H. and E. Blake iii Acknowledgements As my six years as a graduate student in Hawaii draws to a close, I'm grateful to a wide range of individuals who have made this thesis possible. Without a broad network of support and enthusiasm for my research, obtaining this degree would not have been possible. A famous scientist once said, "If I have seen further it is by standing on the shoulders of Giants." Though my achievements certainly pale in comparison, the sentiment rings true to my work. Thank you to all of you who helped me get to this point{it wouldn't have happened without you. First, I'd like to acknowledge the support of the US taxpayers. Without the funding that all of us provide, the NASA and NSF funds used to pay my salary would not be available. I'd also like to thank the citizens of the state of Hawaii. Your (retroactive) choice to allow scientific research at the summit of Maunakea was essential to the success of this research. Given the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawai`ian community, I am very grateful to have been given the opportunity to use this unique place to best further exoplanet and astronomical studies for the common good. -
From ESPRESSO to PLATO: Detecting and Characterizing Earth-Like Planets in the Presence of Stellar Noise
From ESPRESSO to PLATO: detecting and characterizing Earth-like planets in the presence of stellar noise Tese de Doutouramento Luisa Maria Serrano Departamento de Fisica e Astronomia do Porto, Faculdade de Ciências da Universidade do Porto Orientador: Nuno Cardoso Santos, Co-Orientadora: Susana Cristina Cabral Barros March 2020 Dedication This Ph.D. thesis is the result of 4 years of work, stress, anxiety, but, over all, fun, curiosity and desire of exploring the most hidden scientific discoveries deserved by Astrophysics. Working in Exoplanets was the beginning of the realization of a life-lasting dream, it has allowed me to enter an extremely active and productive group. For this reason my thanks go, first of all, to the ’boss’ and my Ph.D. supervisor, Nuno Santos. He allowed me to be here and introduced me in this world, a distant mirage for the master student from a university where there was no exoplanets thematic line. I also have to thank him for his humanity, not a common quality among professors. The second thank goes to Susana, who was always there for me when I had issues, not necessarily scientific ones. I finally have to thank Mahmoud; heis not listed as supervisor here, but he guided me, teaching me how to do research and giving me precious life lessons, which made me growing. There is also a long series of people I am thankful to, for rendering this years extremely interesting and sustaining me in the deepest moments. My first thought goes to my parents: they were thousands of kilometers far away from me, though they never left me alone and they listened to my complaints, joy, sadness...everything.