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The University of Chicago Glimpses of Far Away
THE UNIVERSITY OF CHICAGO GLIMPSES OF FAR AWAY PLACES: INTENSIVE ATMOSPHERE CHARACTERIZATION OF EXTRASOLAR PLANETS A DISSERTATION SUBMITTED TO THE FACULTY OF THE DIVISION OF THE PHYSICAL SCIENCES IN CANDIDACY FOR THE DEGREE OF DOCTOR OF PHILOSOPHY DEPARTMENT OF ASTRONOMY AND ASTROPHYSICS BY LAURA KREIDBERG CHICAGO, ILLINOIS AUGUST 2016 Copyright c 2016 by Laura Kreidberg All Rights Reserved Far away places with strange sounding names Far away over the sea Those far away places with strange sounding names Are calling, calling me. { Joan Whitney & Alex Kramer TABLE OF CONTENTS LIST OF FIGURES . vii LIST OF TABLES . ix ACKNOWLEDGMENTS . x ABSTRACT . xi 1 INTRODUCTION . 1 1.1 Exoplanets' Greatest Hits, 1995 - present . 1 1.2 Moving from Discovery to Characterization . 2 1.2.1 Clues from Planetary Atmospheres I: How Do Planets Form? . 2 1.2.2 Clues from Planetary Atmospheres II: What are Planets Like? . 3 1.2.3 Goals for This Work . 4 1.3 Overview of Atmosphere Characterization Techniques . 4 1.3.1 Transmission Spectroscopy . 5 1.3.2 Emission Spectroscopy . 5 1.4 Technical Breakthroughs Enabling Atmospheric Studies . 7 1.5 Chapter Summaries . 10 2 CLOUDS IN THE ATMOSPHERE OF THE SUPER-EARTH EXOPLANET GJ 1214b . 12 2.1 Introduction . 12 2.2 Observations and Data Reduction . 13 2.3 Implications for the Atmosphere . 14 2.4 Conclusions . 18 3 A PRECISE WATER ABUNDANCE MEASUREMENT FOR THE HOT JUPITER WASP-43b . 21 3.1 Introduction . 21 3.2 Observations and Data Reduction . 23 3.3 Analysis . 24 3.4 Results . 27 3.4.1 Constraints from the Emission Spectrum . -
![Arxiv:1406.5253V1 [Astro-Ph.EP] 20 Jun 2014](https://docslib.b-cdn.net/cover/7421/arxiv-1406-5253v1-astro-ph-ep-20-jun-2014-817421.webp)
Arxiv:1406.5253V1 [Astro-Ph.EP] 20 Jun 2014
Physical Properties of Near-Earth Asteroid 2011 MD M. Mommert Department of Physics and Astronomy, Northern Arizona University, PO Box 6010, Flagstaff, AZ 86011, USA D. Farnocchia Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA J. L. Hora Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA S. R. Chesley Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA D. E. Trilling Department of Physics and Astronomy, Northern Arizona University, PO Box 6010, Flagstaff, AZ 86011, USA P. W. Chodas Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA arXiv:1406.5253v1 [astro-ph.EP] 20 Jun 2014 M. Mueller SRON Netherlands Institute for Space Research, Postbus 800, 9700 AV, Groningen, The Netherlands A. W. Harris DLR Institute of Planetary Research, Rutherfordstrasse 2, 12489 Berlin, Germany H. A. Smith –2– Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA and G. G. Fazio Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138-1516, USA Received ; accepted accepted by ApJL –3– ABSTRACT We report on observations of near-Earth asteroid 2011 MD with the Spitzer Space Telescope. We have spent 19.9 h of observing time with channel 2 (4.5 µm) of the Infrared Array Camera and detected the target within the 2σ positional uncertainty ellipse. Using an asteroid thermophysical model and a model of non- gravitational forces acting upon the object we constrain the physical properties of 2011 MD, based on the measured flux density and available astrometry data. -
Detecting the Yarkovsky Effect Among Near-Earth Asteroids From
Detecting the Yarkovsky effect among near-Earth asteroids from astrometric data Alessio Del Vignaa,b, Laura Faggiolid, Andrea Milania, Federica Spotoc, Davide Farnocchiae, Benoit Carryf aDipartimento di Matematica, Universit`adi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy bSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy cIMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universits, UPMC Univ. Paris 06, Univ. Lille, 77 av. Denfert-Rochereau F-75014 Paris, France dESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy eJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109 CA, USA fUniversit´eCˆote d’Azur, Observatoire de la Cˆote d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, Nice, France Abstract We present an updated set of near-Earth asteroids with a Yarkovsky-related semi- major axis drift detected from the orbital fit to the astrometry. We find 87 reliable detections after filtering for the signal-to-noise ratio of the Yarkovsky drift esti- mate and making sure the estimate is compatible with the physical properties of the analyzed object. Furthermore, we find a list of 24 marginally significant detec- tions, for which future astrometry could result in a Yarkovsky detection. A further outcome of the filtering procedure is a list of detections that we consider spurious because unrealistic or not explicable with the Yarkovsky effect. Among the smallest asteroids of our sample, we determined four detections of solar radiation pressure, in addition to the Yarkovsky effect. As the data volume increases in the near fu- ture, our goal is to develop methods to generate very long lists of asteroids with reliably detected Yarkovsky effect, with limited amounts of case by case specific adjustments. -
Habitability of the Early Earth: Liquid Water Under a Faint Young Sun Facilitated by Strong Tidal Heating Due to a Nearby Moon
Habitability of the early Earth: Liquid water under a faint young Sun facilitated by strong tidal heating due to a nearby Moon Ren´eHeller · Jan-Peter Duda · Max Winkler · Joachim Reitner · Laurent Gizon Draft July 9, 2020 Abstract Geological evidence suggests liquid water near the Earths surface as early as 4.4 gigayears ago when the faint young Sun only radiated about 70 % of its modern power output. At this point, the Earth should have been a global snow- ball. An extreme atmospheric greenhouse effect, an initially more massive Sun, release of heat acquired during the accretion process of protoplanetary material, and radioactivity of the early Earth material have been proposed as alternative reservoirs or traps for heat. For now, the faint-young-sun paradox persists as one of the most important unsolved problems in our understanding of the origin of life on Earth. Here we use astrophysical models to explore the possibility that the new-born Moon, which formed about 69 million years (Myr) after the ignition of the Sun, generated extreme tidal friction { and therefore heat { in the Hadean R. Heller Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 G¨ottingen, Germany E-mail: [email protected] J.-P. Duda G¨ottingenCentre of Geosciences, Georg-August-University G¨ottingen, 37077 G¨ottingen,Ger- many E-mail: [email protected] M. Winkler Max Planck Institute for Extraterrestrial Physics, Giessenbachstraße 1, 85748 Garching, Ger- many E-mail: [email protected] J. Reitner G¨ottingenCentre of Geosciences, Georg-August-University G¨ottingen, 37077 G¨ottingen,Ger- many G¨ottingenAcademy of Sciences and Humanities, 37073 G¨ottingen,Germany E-mail: [email protected] L. -
Meteoroid Impacts Onto Asteroids: a Competitor for Yarkovsky and YORP
Meteoroid impacts onto asteroids: a competitor for Yarkovsky and YORP Paul A. Wiegert Dept. of Physics and Astronomy, The University of Western Ontario, London Ontario CANADA Submitted to Icarus July 14 2014 Abstract The impact of a meteoroid onto an asteroid transfers linear and angular mo- mentum to the larger body, which may affect its orbit and its rotational state. Here we show that the meteoroid environment of our Solar System can have an effect on small asteroids that is comparable to the Yarkovsky and Yarkovsky- O’Keefe-Radzievskii-Paddack (YORP) effects under certain conditions. The momentum content of the meteoroids themselves is expected to generate an effect much smaller than that of the Yarkovsky effect. However, momentum transport by ejecta may increase the net effective force by two orders of magni- tude for impacts into bare rock surfaces. This result is sensitive to the extrapola- tion of laboratory microcratering experiment results to real meteoroid-asteroid collisions and needs further study. If this extrapolation holds, then meteoroid impacts are more important to the dynamics of small asteroids than had previ- ously been considered. Asteroids orbiting on prograde orbits near the Earth encounter an anisotropic arXiv:1407.3714v1 [astro-ph.EP] 14 Jul 2014 meteoroid environment, including a population of particles on retrograde orbits generally accepted to be material from long-period comets spiralling inwards under Poynting-Robertson drag. High relative speed (60 km/s) impacts by me- teoroids provide a small effective drag force that decreases asteroid semimajor axes and which is independent of their rotation pole. This effect may exceed the instantaneous Yarkovsky drift at sizes near and below one meter. -
2010-2011 Top Age Group Times
USA Swimming, Inc. For Dates 9/1/2010 - 8/31/2011 Girls Age 11 50 Freestyle Short Course Yards Power Rank Time Points Name Age LSC / Club Meet Date Meet 1 24.88 906 Harnish, Courtney 11 MA York YMCA 3/11/2011 2011 MA SC Junior Olympics 2 25.18 881 Wittmer, Rachel 11 MN Aquajets Swim Team 3/11/2011 2011 MN MCA Age Group State Me 3 25.21 879 Grout, Morgan 11 IN Carmel Swim Club 3/18/2011 2011 IN Age Group State - 4 25.26 874 McGowan, Alessia 11 MR Asphalt Green Unified Aquatics 2/19/2011 2011 MR Zone Team Qualifier 5 25.41 862 Wall, Ingrid 11 FL T2 Aquatics 12/10/2010 2010 IL WILD TYR WINTER BLAST 6 25.49 855 Harvard, Laurynn 11 IL Wheaton Swim Club, Inc. 3/11/2011 2011 IL SCY ISI Age Group Cham 7 25.61 845 Vanhoven, Lexus 11 MI East Grand Rapids Aquatics 3/11/2011 2011 MI WMS/WOSC 12 & U STATE 8 25.62 845 Palochik, Victoria 11 MA Unattached 3/12/2011 2011 MA AP YMCA PA East District 9 25.64 843 Suer, Samantha 11 NI Chenango Aquatic Swim Club 4/6/2011 2011 FL CAT/NASA Showcase 10 25.65 842 Kraus, Alena 11 FL Makos Aquatics Club of Gainesville 3/26/2011 2011 FL vs. FGC All-Star Meet Girls Age 11 100 Freestyle Short Course Yards Power Rank Time Points Name Age LSC / Club Meet Date Meet 1 53.60 935 Harnish, Courtney 11 MA York YMCA 3/10/2011 2011 MA SC Junior Olympics 2 54.80 882 Grout, Morgan 11 IN Carmel Swim Club 3/18/2011 2011 IN Age Group State - 3 54.95 875 Pfeifer, Evie 11 OZ Parkway Swim Club 2/25/2011 2011 OZ Division I Champs 4 55.25 862 Palochik, Victoria 11 MA Unattached 3/10/2011 2011 MA SC Junior Olympics 5 55.26 862 Suer, Samantha 11 NI Chenango Aquatic Swim Club 3/17/2011 2011 NI - Niagara LSC Championships 6 55.40 856 Romano, Kristen 11 NI Town Wrecker Swim Team 3/17/2011 2011 NI - Niagara LSC Championships 7 55.41 855 Rongione, Isabella 11 PV The Fish 4/6/2011 2011 FL CAT/NASA Showcase 8 55.76 840 Joassaint, Britheny 11 GA Marietta Marlins, Inc 2/25/2011 2011 GA 14&U Short Course 9 55.80 839 Crouse, Eva 11 CT University Aquatic Club 3/10/2011 2011 CT Age Group Championship SCY Page 1 of 61 USA Swimming, Inc. -
Jjmonl 1612.Pmd
alactic Observer GJohn J. McCarthy Observatory Volume 9, No. 12 December 2016 Water - the elusive elixir of life in the cosmos - Is it even closer than we thought? The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky It is through their efforts that the McCarthy Observatory Technical Support has established itself as a significant educational and Bob Lambert recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Allison Tom Heydenburg Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Randy Finden Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue "OUT THE WINDOW ON YOUR LEFT"............................... 3 COMMONLY USED TERMS .............................................. 17 TAURUS-LITTROW .......................................................... 3 EARTH-SUN LAGRANGE POINTS & JAMES WEBB TELESCOPE 17 OVER THE TOP ............................................................... 4 REFERENCES ON DISTANCES ........................................ -
Chodas-MFR Observations Releasable Final2.Pptx
Asteroid Redirect Robotic Mission (ARRM): Observation Campaign Study Paul Chodas, NASA NEO Program Office With assistance from: Lindley Johnson (HQ), Robert Jedicke and Eva Schunova (U. of Hawaii), Bob Gershman, Mike Hicks, Steve Chesley, Don Yeomans (JPL) Executive Summary • Current population models suggest that there are a large number of good ARRM candidate targets, but current surveys are finding only 2 to 3 per year, and only 4 of the known candidates can be adequately characterized (2009 BD, 2011 MD, 2013 EC20, 2008 HU4). • Discovery of good candidates is challenging, but the rate can be increased to at least 5 per year via near-term enhancements to current survey assets, as well as additional assets that can be online by 2015. • Enhancing surveys to find more ARRM candidates also increases their capabilities for finding potentially hazardous asteroids in general. • The discovery process alone is not sufficient to identify good candidates: physical characterization is also needed, particularly re size and mass. • Radar is a key characterization asset for ARRM candidates. • Rapid response is critical for physical characterization of newly discovered ARRM candidates. The process has been successfully exercised for a small candidate asteroid. Asteroid Redirect Mission • Mission Formulation Review • For Public Release 2 Numbers of Near-Earth Asteroids (NEAs) • 99% of Near-Earth Objects are asteroids (NEAs). • Current number of known NEAs: ~10,000, discovered at a rate of ~1000 per year. • Since 1998, NASA’s NEO Observation Program has led the international NEO discovery and characterization effort; this responsibility should continue in the search for smaller asteroids. • 95% of 1-km and larger NEAs have been found; the completion percentage drops for smaller asteroids because the population increases exponentially as size decreases. -
NASA APR APP Part 3
Part 3—Performance Reporting and Planning Introduction Part 3 presents NASA’s integrated FY 2014 Annual Performance Report, FY 2015 Annual Performance Plan Update, and FY 2016 Annual Performance Plan. It features a summary of NASA’s first-ever Strategic Review by strategic objective, with strategic objective-level performance ratings selected by NASA in consultation with the Office of Management and Budget (OMB). It also shows up to six years of historical rated performance alongside two years of future plans. Together this information provides a retrospective and prospective view of NASA’s performance. The integrated report contains the following: Charts summarizing performance goal and annual performance indicator ratings, organized by strategic goal. A summary of the annual Strategic Review by strategic objective. The section below provides an overview of the strategic objective content. The strategic objective’s budget, actuals from FY 2014, the budget request for FY 2016, and notional funding through FY 2020. The performance goals contributing to the strategic objective. Each performance goal includes an FY 2014 performance rating, multiyear performance trends beginning with FY 2011,3 any planned performance changes for FY 2015 or FY 2016, a narrative describing activities contributing to performance progress in FY 2014, and an improvement plan for performance goals rated yellow or red. Figure 15 is a quick guide to the performance tables. The annual performance indicators associated with the performance goal, including the FY 2014 performance rating, multiyear performance trends beginning with FY 2009, the planned performance for FY 2015 and FY 2016, and a performance explanation for annual performance indicators rated yellow or red. -
DISTANT Ekos
Issue No. 92 April 2014 ✤✜r s ✓✏ DISTANT EKO ❞✐ ✒✑ The Kuiper Belt Electronic Newsletter ✣✢ Edited by: Joel Wm. Parker [email protected] www.boulder.swri.edu/ekonews CONTENTS News & Announcements ................................. 2 Abstracts of 9 Accepted Papers ......................... 3 Titles of 3 Submitted Papers ........................... .10 Titles of 1 Other Paper of Interest ...................... 10 Conference Information .............................. 11 Newsletter Information .............................. 12 1 NEWS & ANNOUNCEMENTS There were 3 new TNO discoveries announced since the previous issue of Distant EKOs: 2011 HJ103, 2012 HZ84, 2012 XR157 and 10 new Centaur/SDO discoveries: 2011 HK103, 2012 VP113, 2013 FY27, 2013 FZ27, 2013 LU35, 2014 DT112, 2014 FW, 2014 FX43, 2014 GE45, 2014 HY123 Reclassified objects: 2010 GF65 (SDO → Centaur) 2012 GX17 (Centaur → SDO) 2014 FW (Centaur → SDO) 2013 FZ27 (SDO → TNO) Objects recently assigned numbers: 2011 WU92 = (389820) Objects recently assigned names: 2003 QW111 = Manwe Current number of TNOs: 1263 (including Pluto) Current number of Centaurs/SDOs: 393 Current number of Neptune Trojans: 9 Out of a total of 1665 objects: 644 have measurements from only one opposition 631 of those have had no measurements for more than a year 326 of those have arcs shorter than 10 days (for more details, see: http://www.boulder.swri.edu/ekonews/objects/recov_stats.jpg) 2 PAPERS ACCEPTED TO JOURNALS A Sedna-like Body with a Perihelion of 80 Astronomical Units C. Trujillo1 and S. Sheppard2 1 Gemini Observatory, 670 North A‘ohoku Place, Hilo, HI 96720, USA 2 Carnegie Institution for Science, 5241 Broad Branch Road NW, Washington, DC 20015, USA The observable Solar System can be divided into three distinct regions: the rocky terrestrial planets including the asteroids at 0.39 to 4.2 astronomical units (AU) from the Sun (where 1 AU is the mean distance between Earth and the Sun), the gas giant planets at 5 to 30 AU from the Sun, and the icy Kuiper belt objects at 30 to 50 AU from the Sun. -
Number Worked As Current Name Vol-Num Pg # Authors 1 Ceres 42-2 94 Melillo, F
The "Worked As" column gives the name/designation used in the original article. If the object was subsequently named, the "Current Name" column gives the name currently in the MPCORB file. The page number gives the first page of the article in which the object appears. Only those references that include lightcurves, other photometric data, and/or shape/spin axis models are included. Number Worked As Current Name Vol-Num Pg # Authors 1 Ceres 42-2 94 Melillo, F. J. 2 Pallas 35-2 63 Higley, S. et al. (Shape/Spin Models) 5 Astraea 35-2 63 Higley, S. et al. (Shape/Spin Models) 8 Flora 36-4 133 Pilcher, F. 9 Metis 36-3 98 Timerson, B. et al. 10 Hygiea 47-2 133 Picher, F. 10 Hygiea 48-2 166 Ferrais, M. et al. 11 Parthenope 37-3 119 Pilcher, F. 11 Parthenope 38-4 183 Pilcher, F. 12 Victoria 40-3 161 Pilcher, F. 12 Victoria 42-2 94 Melillo, F. J. 13 Egeria 36-4 133 Pilcher, F. 14 Irene 36-4 133 Pilcher, F. 14 Irene 39-3 179 Aymani, J.M. 16 Psyche 38-4 200 Timerson, B. et al. 16 Psyche 43-2 137 Warner, B. D. 17 Thetis 34-4 113 Warner, B.D. (H-G, Color Index) 18 Melpomene 40-1 33 Pilcher, F. 18 Melpomene 41-3 155 Pilcher, F. 19 Fortuna 36-3 98 Timerson, B. et al. 22 Kalliope 30-2 27 Trigo-Rodriguez, J.M. 22 Kalliope 34-3 53 Gungor, C. 22 Kalliope 34-3 56 Alton, K.B. -
Analysis and Selection of Optimal Targets for a Planetary Defense Technology Demonstration Mission
Analysis and Selection of Optimal Targets for a Planetary Defense Technology Demonstration Mission Sam Wagner, ∗ Tim Winkler, y and Bong Wie z Asteroid Deflection Research Center, Iowa State University, Ames, IA, USA In the past; various options have been proposed for mitigating the impact threat of near-Earth objects (NEOs. This paper presents mission analysis and design to potential NEO candidates for a demonstration of such planetary defense technologies. In particu- lar, a flight demonstration mission is necessary to validate the effectiveness of blending a hypervelocity kinetic impactor with a penetrated nuclear subsurface explosion. Possible asteroid candidates are found by determining optimal missions for several possible mission architectures for nearly 3400 potential asteroids. The optimization is performed using a genetic algorithm developed to solve complex mission design problems. I. Introduction As early as 1992, the idea of discovering and tracking near-Earth objects (NEOs) was proposed to the U.S. Congress.1 The search, called the Spaceguard Survey, was later implemented in 1998 with the ultimate goal of finding 90 percent of the estimated asteroid population of 1 km in diameter or larger by 2008. This survey only intended to find asteroids that were large enough to cause catastrophe on a global scale. While not large enough to affect the entire globe, impacts with objects smaller than 1 km occur more frequently, and cause significant damage upon impact. In 2005, the George E. Brown, Jr. Near-Earth Object Survey Act expanded the search to include the detection and characterization of NEOs as small as 140 m. The new objectives retained the goal of detecting 90 percent of the NEO population, but extended the completion date to the end of 2020.