DOCSLIB.ORG

Proquest Dissertations

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Proquest Dissertations Characterizing transiting extrasolar giant planets: On companions, rings, and love handles Item Type text; Dissertation-Reproduction (electronic) Authors Barnes, Jason Wayne Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 01/10/2021 05:33:59 Link to Item http://hdl.handle.net/10150/290019 NOTE TO USERS This reproduction is the best copy available. UMI CHARACTERIZING TRANSITING EXTRASOLAR GIANT PLANETS: ON COMPANIONS, RINGS, AND LOVE HANDLES by Jason Wayne Barnes A Dissertation Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCES In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 2 0 0 4 UMI Number: 3131584 INFORMATION TO USERS The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleed-through, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. UMI UMI Microform 3131584 Copyright 2004 by ProQuest Information and Learning Company. All rights reserved. This microform edition is protected against unauthorized copying under Title 17, United States Code. ProQuest Information and Learning Company 300 North Zeeb Road P.O. Box 1346 Ann Arbor, Ml 48106-1346 2 The University of Arizona ® Graduate College As members of the Final Examination Committee, we certify that we have read the dissertation prepared by Jason Wayne Barnes entitled Characterizing Transiting Extrasolar Giant Planets: On Compan ions, Rings, and Love Handles and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy ^•27/2 Robert H. Brown "/date ^ C?/( /(pH- WI11iam B. Hubbard date Adatn Showman date Renu Malhotra date r In /gy Ralph Lorenz date Final approval and acceptance of this dissertation is contingent upon the candidate's submission of the fmal copies of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommen^hat it be accepted as fulfilling the dissertation requirement. Dissertation Director: Robert H. Brown / 4ate 3 STATEMENT BY AUTHOR This dissertation has been submitted in partial fulfillment of requirements for an advanced degree at The University of Arizona and is deposited in the Uni­ versity Library to be made available to borrowers under rules of the library. Brief quotations from this dissertation are allowable without special per­ mission, provided that accurate acknowledgment of source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED: 4 ACKNOWLEDGEMENTS I would like to thank a few of the people that had a hand in getting me to my Ph.D.. Firstly I want to thank my parents, Wayne and Nancy Barnes for giving me the caring and questioning start that a proto-scientist needs. My sister Terra Barnes and brother Alexander Barnes shaped my childhood and are now following on in the family business of science. My undergrad research boss at JPL, Vikki Meadows, taught me the astro­ nomical ropes. My advisor, Bob Brown gave me expert advice and was available when I needed him, but allowed me the freedom to pursue my own projects. My fellow grads Oleg Abramov, Jade Bond, Matt Chamberlain, Curtis Cooper, Josh Emery, Jonathan Fortney, Maki Hattori, Windy Jaeger, John Keller, Peter Lanagan, Yuan Lian, Celinda Marsh, Rachel Mastrapa, Moses Milazzo, John Moores, Mandy Proctor, Jani Radebaugh, Jim Richardson, Abby Sheffer, and Matt Tiscareno, but particularly my officemates Dave O'Brien and Fred Ciesla and other members of the incoming LPL Grad class of 1998 Ross Beyer, Terry Hurford and Paul Withers helped keep me sane through my indenture, as have postgrads Barb Cohen, Rob Coker, Carl Hergenrother, Ralph Lorenz, Andy Rivkin, Christian Schaller, and Zibi Turtle. I would also like to thank the faculty and staff in LPL that have helped me with my studies, including Brad Castalia, Joe Plassman, Maria Schuhardt, Rick Greenberg, Bill Hubbard, Renu Malhotra, Jay Melosh, and Adam Showman. I also apreciate the support of those people at Caltech that helped me through to graduation: Chris Bisbee, Christy Edwards, Corinne Gilliam, BJ Horn, Natron Hsu, Pat Jewell, Diana King, Chris Kurtz, Brian Monroe, Donnie Pinkston, Katie Stofer, Keely Walker, and David Winkler. Lastly, I would like to thank my fiancee Gwen Bart for her emotional and intellectual support. 5 DEDICATION for my family 6 TABLE OF CONTENTS LIST OF FIGURES 8 LIST OF TABLES 9 ABSTRACT 10 CHAPTER 1 Introduction 11 1.1 OVERVIEW 11 1.2 DETECTION METHODS 14 1.2.1 Radial Velocity 14 1.2.2 Transit 15 1.2.3 Astrometry 19 1.2.4 Microlensing 20 1.2.5 Direct Detection 21 1.3 THE NEW PLANETS 22 1.3.1 Roasters 22 1.3.2 Eccentric Planets 24 1.3.3 Planets Around High-Metallicity Stars 25 1.3.4 Multiple-Planet Systems 25 1.3.5 Jupiter Analogs 26 1.4 TRANSIT CHARACTERIZATION OF EGPs 26 CHAPTER 2 Extrasolar Moons 29 2.1 INTRODUCTION 29 2.2 TIDAL THEORY AND METHODS 30 2.3 CONSTRAINTS ON SATELLITE MASSES 32 2.3.1 Analytical Treatment 36 2.3.2 Numerical Treatment 38 2.4 IMPLICATIONS 40 2.4.1 Known Extrasolar Planets 40 2.4.2 Earth-like Moons 43 2.4.3 Future Discoveries 45 CHAPTER 3 Extrasolar Oblateness 46 3.1 INTRODUCTION 46 3.2 EXOPLANETS AND ROTATION 47 3.2.1 Tidally Unaffected 48 3.2.2 Tidally Influenced 49 7 TABLE OF CONTENTS — Continued 3.2.3 Tidally Dominated 50 3.3 ROTATION AND OBLATENESS 51 3.4 OBLATENESS AND TRANSIT LIGHTCURVES 58 3.4.1 Transit Anatomy 58 3.4.2 Methods 60 3.4.3 Results 61 3.5 TRANSIT LIGHTCURVES AND EXOPLANETS 64 3.5.1 Zero Obliquity 64 3.5.2 Nonzero Obliquity 73 3.6 CONCLUSIONS 76 CHAPTER 4 Extrasolar Rings 78 4.1 INTRODUCTION 78 4.2 MOTIVATION 80 4.2.1 Rings in the Solar System 80 4.2.2 Rings in Extrasolar Systems 83 4.3 EXTINCTION 84 4.3.1 Methods 84 4.3.2 Results 86 4.4 DIFFRACTION 95 4.4.1 Theory 95 4.4.2 Results 98 4.5 APPLICATION 106 4.6 CONCLUSION 108 CHAPTER 5 CONCLUSION 110 5.1 Moons 110 5.2 Lightcurve Deviations 112 APPENDIX A Extrasolar Planet and Parent Star Data 115 REFERENCES 122 8 LIST OF FIGURES 1.1 The Radial Velocity and Extrasolar Planets 13 2.1 a versus time for tidally evolving moons 35 2.2 Satellite stability diagram 39 2.3 Stability of Earth-like moons 44 3.1 Equilibrium Spin:Orbit Ratio as a Function of Orbital Eccentricity . 52 3.2 Moment of Inertia Coefficients for Giant Planets 56 3.3 Transit Schematic 59 3.4 Incorrect Detectability of Oblateness 62 3.5 Detectability of Oblateness for Zero-Obliquity Planets: Four Parameter Model 66 3.6 Detectability of Oblateness for Zero-Obliquity Planets: Five Parameter Model 67 3.7 Best-Fit Spherical Planet Transit Parameters 71 3.8 Change in Fitted Parameters as a Function of Impact Parameter .... 72 3.9 Detectability of Oblateness for Nonzero Obliquity 74 4.1 Symmetric Ring Detectability 88 4.2 Asymmetric Ring Detectability 89 4.3 Transit Geometry Schematic 90 4.4 Scattering vs Ring Particle Size 99 4.5 Symmetric Ring Detectability 100 4.6 Scattering Ring Detectability 102 4.7 Diffraction Footprint 104 4.8 Saturn Ring Detectability 107 9 LIST OF TABLES 2.1 Solar System Satellite Semimajor Axes 33 2.2 Constraints on Satellites around Selected Extrasolar Planets 42 3.1 Darwin-Radau in the Solar System 54 A.l Extrasolar Giant Planet Data 116 A.2 Extrasolar Giant Planet Data II 117 A.3 Extrasolar Giant Planet Data III 118 A.4 Extrasolar Giant Planet Parent Star Data 119 A.5 Extrasolar Giant Planet Parent Star Data II 120 A.6 Extrasolar Giant Planet Parent Star Data III 121 10 ABSTRACT For my Ph.D. research I investigated the prospects for characterizing transiting extrasolar giant planets from their transit lightcurves. Hubble Space Telescope photometry of transiting planet HD209458b revealed that the planet has no moons. Here, I show that tidal orbital evolution of moons limits their lifetimes, and hence that no moons larger than Amalthea in size should survive around HD209458b, consistent with observations. 1 then calculate the detectability and scientific po­ tential of planetary rings and oblateness. Oblateness will prove difficult to reliably detect, even with the Hubble Space Telescope. However, large Saturn-like ring sys­ tems should be easy to find around transiting extrasolar giant planets if such rings exist. 11 CHAPTER 1 Introduction 1.1 OVERVIEW In October of 1995, Mayor and Queloz (1995) announced the discovery of the first planet orbiting a main-sequence star other than the Sun. Mayor and Queloz found extrasolar planet 51 Pegasus b by precisely monitoring the radial velocity of its parent star, 51 Pegasus.
Load more

Recommended publications
  • Where Are the Distant Worlds? Star Maps
    W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star.
    [Show full text]
  • Titan and Enceladus $1 B Mission
    JPL D-37401 B January 30, 2007 Titan and Enceladus $1B Mission Feasibility Study Report Prepared for NASA’s Planetary Science Division Prepared By: Kim Reh Contributing Authors: John Elliott Tom Spilker Ed Jorgensen John Spencer (Southwest Research Institute) Ralph Lorenz (The Johns Hopkins University, Applied Physics Laboratory) KSC GSFC ARC Approved By: _________________________________ Kim Reh Dr. Ralph Lorenz Jet Propulsion Laboratory The Johns Hopkins University, Applied Study Manager Physics Laboratory Titan Science Lead _________________________________ Dr. John Spencer Southwest Research Institute Enceladus Science Lead Pre-decisional — For Planning and Discussion Purposes Only Titan and Enceladus Feasibility Study Report Table of Contents JPL D-37401 B The following members of an Expert Advisory and Review Board contributed to ensuring the consistency and quality of the study results through a comprehensive review and advisory process and concur with the results herein. Name Title/Organization Concurrence Chief Engineer/JPL Planetary Flight Projects Gentry Lee Office Duncan MacPherson JPL Review Fellow Glen Fountain NH Project Manager/JHU-APL John Niehoff Sr. Research Engineer/SAIC Bob Pappalardo Planetary Scientist/JPL Torrence Johnson Chief Scientist/JPL i Pre-decisional — For Planning and Discussion Purposes Only Titan and Enceladus Feasibility Study Report Table of Contents JPL D-37401 B This page intentionally left blank ii Pre-decisional — For Planning and Discussion Purposes Only Titan and Enceladus Feasibility Study Report Table of Contents JPL D-37401 B Table of Contents 1. EXECUTIVE SUMMARY.................................................................................................. 1-1 1.1 Study Objectives and Guidelines............................................................................ 1-1 1.2 Relation to Cassini-Huygens, New Horizons and Juno.......................................... 1-1 1.3 Technical Approach...............................................................................................
    [Show full text]
  • 1999-2000 Annual Report
    Anglo-Australian Observatory Annual Report of the Anglo-Australian Telescope Board 1 July 1999 to 30 June 2000 ANGLO-AUSTRALIAN OBSERVATORY PO Box 296, Epping, NSW 1710, Australia 167 Vimiera Road, Eastwood, NSW 2122, Australia PH (02) 9372 4800 (international) + 61 2 9372 4800 FAX (02) 9372 4880 (international) + 61 2 9372 4880 e-mail [email protected] ANGLO-AUSTRALIAN TELESCOPE BOARD PO Box 296, Epping, NSW 1710, Australia 167 Vimiera Road, Eastwood, NSW 2122, Australia PH (02) 9372 4813 (international) + 61 2 9372 4813 FAX (02) 9372 4880 (international) + 61 2 9372 4880 e-mail [email protected] ANGLO-AUSTRALIAN TELESCOPE/UK SCHMIDT TELESCOPE PriVate Bag, Coonabarabran, NSW 2357, Australia PH (02) 6842 6291 (international) + 61 2 6842 6291 AAT FAX (02) 6884 2298 (international) + 61 2 6884 298 UKST FAX (02) 6842 2288 (international) + 61 2 6842 2288 WWW http://www.aao.gov.au/ © Anglo-Australian Telescope Board 2000 ISSN 1443-8550 COVER: A digital image of the Antennae galaxies (NGC4038-39) made by combining three images from the Tek2 CCD on the AAT (Steve Lee and David Malin). A new wide field CCD Imager (WFI) will come into use in 2000 and will enable many more images like this to be made. COVER DESIGN: Encore International COMPUTER TYPESET AT THE: Anglo-Australian ObserVatory ii The Right Honourable Stephen Byers, MP, President of the Board of Trade and Secretary of State for Trade and Industry, Government of the United Kingdom of Great Britain and Northern Ireland The Honourable Dr David Kemp, MP, Minister for Education, Training and Youth Affairs GoVernment of the Commonwealth of Australia In accordance with Article 8 of the Agreement between the Australian GoVernment and the GoVernment of the United Kingdom to proVide for the establishment and operation of an optical telescope at Siding Spring Mountain in the state of New South Wales, I present herewith a report by the Anglo-Australian Telescope Board for the year from 1 July 1999 to 30 June 2000.
    [Show full text]
  • A Guide to Smartphone Astrophotography National Aeronautics and Space Administration
    National Aeronautics and Space Administration A Guide to Smartphone Astrophotography National Aeronautics and Space Administration A Guide to Smartphone Astrophotography A Guide to Smartphone Astrophotography Dr. Sten Odenwald NASA Space Science Education Consortium Goddard Space Flight Center Greenbelt, Maryland Cover designs and editing by Abbey Interrante Cover illustrations Front: Aurora (Elizabeth Macdonald), moon (Spencer Collins), star trails (Donald Noor), Orion nebula (Christian Harris), solar eclipse (Christopher Jones), Milky Way (Shun-Chia Yang), satellite streaks (Stanislav Kaniansky),sunspot (Michael Seeboerger-Weichselbaum),sun dogs (Billy Heather). Back: Milky Way (Gabriel Clark) Two front cover designs are provided with this book. To conserve toner, begin document printing with the second cover. This product is supported by NASA under cooperative agreement number NNH15ZDA004C. [1] Table of Contents Introduction.................................................................................................................................................... 5 How to use this book ..................................................................................................................................... 9 1.0 Light Pollution ....................................................................................................................................... 12 2.0 Cameras ................................................................................................................................................
    [Show full text]
  • Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
    Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis,
    [Show full text]
  • Ralph Lorenz Johns Hopkins – Applied Physics Lab
    Space phySicS Seminar Ralph Lorenz Johns Hopkins – Applied Physics Lab Sailing the Seas of Titan, Saturn's Earth-Like Moon Thursday, September 19, 2013 725 Commonwealth Ave. Refreshments at 3:30pm in CAS 500 Talk begins at 4:00pm in CAS 502 Abstract: Oceanography is no longer just an Earth Science. The ongoing NASA/ESA Cassini mission - still making exciting discoveries 10 years after its arrival in the rich Saturnian system - has found that three seas of liquid hydrocarbons adorn Saturn’s giant, frigid moon Titan. Titan was already exotic, having a thick, organic-rich atmosphere, and a diverse landscape with mountains, craters, river channels and vast fields of sand dunes, but these seas, and hundreds of lakes, present a new environment (low gravity, dense atmosphere, hydrocarbon liquid) in which to explore familiar and important physical processes such as air:sea heat and moisture exchange, wind- driven currents and waves, etc. Moreover, Titan’s seas (notably the two largest ones, Kraken Mare and Ligiea Mare, about 1000km and 400km across, respectively) offer an appealing and accessible target for future Titan exploration. This talk will review the latest findings from Cassini, and its prospects for new discoveries as we move towards Titan’s northern summer solstice in 2017, and the opportunities for future exploration which might include (as at Mars) orbiters and landers, but also vehicles that can exploit Titan’s environment such as balloons or airplanes. The most affordable near-term prospect for in-situ exploration is a capsule to float in the seas of Titan, where after splashdown it would drift in the winds to make a traverse across the sea, measuring the liquid composition and turbidity, studying conditions with cameras and meteorological instruments, and exploring the seabed with a depth sounder.
    [Show full text]
  • Titan a Moon with an Atmosphere
    TITAN A MOON WITH AN ATMOSPHERE Ashley Gilliam Earth 450 – Satellites of Jupiter and Saturn 4/29/13 SATURN HAS > 60 SATELLITES, WHY TITAN? Is the only satellite with a dense atmosphere Has a nitrogen-rich atmosphere resembles Earth’s Is the only world besides Earth with a liquid on its surface • Possible habitable world Based on its size… Titan " a planet in its o# $ght! R = 6371 km R = 2576 km R = 1737 km Ch$%iaan Huy&ns (1629-1695) DISCOVERY OF TITAN Around 1650, Huygens began building telescopes with his brother Constantijn On March 25, 1655 Huygens discovered Titan in an attempt to study Saturn’s rings Named the moon Saturni Luna (“Saturns Moon”) Not properly named until the mid-1800’s THE DISCOVERY OF TITAN’S ATMOSPHERE Not much more was learned about Titan until the early 20th century In 1903, Catalan astronomer José Comas Solà claimed to have observed limb darkening on Titan, which requires the presence of an atmosphere Gerard P. Kuiper (1905-1973) José Comas Solà (1868-1937) This was confirmed by Gerard Kuiper in 1944 Image Credit: Ralph Lorenz Voyager 1 Launched September 5, 1977 M"sions to Titan Pioneer 11 Launched April 6, 1973 Cassini-Huygens Images: NASA Launched October 15, 1997 Pioneer 11 Could not penetrate Titan’s Atmosphere! Image Credit: NASA Vo y a &r 1 Image Credit: NASA Vo y a &r 1 What did we learn about the Atmosphere? • Composition (N2, CH4, & H2) • Variation with latitude (homogeneously mixed) • Temperature profile Mesosphere • Pressure profile Stratosphere Troposphere Image Credit: Fulchignoni, et al., 2005 Image Credit: Conway et al.
    [Show full text]
  • DAVINCI: Deep Atmosphere Venus Investigation of Noble Gases, Chemistry, and Imaging Lori S
    DAVINCI: Deep Atmosphere Venus Investigation of Noble gases, Chemistry, and Imaging Lori S. Glaze, James B. Garvin, Brent Robertson, Natasha M. Johnson, Michael J. Amato, Jessica Thompson, Colby Goodloe, Dave Everett and the DAVINCI Team NASA Goddard Space Flight Center, Code 690 8800 Greenbelt Road Greenbelt, MD 20771 301-614-6466 Lori.S.Glaze@ nasa.gov Abstract—DAVINCI is one of five Discovery-class missions questions as framed by the NRC Planetary Decadal Survey selected by NASA in October 2015 for Phase A studies. and VEXAG, without the need to repeat them in future New Launching in November 2021 and arriving at Venus in June of Frontiers or other Venus missions. 2023, DAVINCI would be the first U.S. entry probe to target Venus’ atmosphere in 45 years. DAVINCI is designed to study The three major DAVINCI science objectives are: the chemical and isotopic composition of a complete cross- section of Venus’ atmosphere at a level of detail that has not • Atmospheric origin and evolution: Understand the been possible on earlier missions and to image the surface at origin of the Venus atmosphere, how it has evolved, optical wavelengths and process-relevant scales. and how and why it is different from the atmospheres of Earth and Mars. TABLE OF CONTENTS • Atmospheric composition and surface interaction: Understand the history of water on Venus and the 1. INTRODUCTION ....................................................... 1 chemical processes at work in the lower atmosphere. 2. MISSION DESIGN ..................................................... 2 • Surface properties: Provide insights into tectonic, 3. PAYLOAD ................................................................. 2 volcanic, and weathering history of a typical tessera 4. SUMMARY ................................................................ 3 (highlands) terrain.
    [Show full text]
  • Scientific Observations with the Insight Solar Arrays: Dust, Clouds
    Scientific Observations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars Ralph Lorenz, Mark Lemmon, Justin Maki, Donald Banfield, Aymeric Spiga, Constantinos Charalambous, Elizabeth Barrett, Jennifer Herman, Brett White, Samuel Pasco, et al. To cite this version: Ralph Lorenz, Mark Lemmon, Justin Maki, Donald Banfield, Aymeric Spiga, et al.. Scientific Obser- vations With the InSight Solar Arrays: Dust, Clouds, and Eclipses on Mars. Earth and Space Science, American Geophysical Union/Wiley, 2020, 7 (5), 10.1029/2019EA000992. hal-02872154 HAL Id: hal-02872154 https://hal.sorbonne-universite.fr/hal-02872154 Submitted on 17 Jun 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Distributed under a Creative Commons Attribution - NonCommercial - NoDerivatives| 4.0 International License RESEARCH ARTICLE Scientific Observations With the InSight Solar Arrays: 10.1029/2019EA000992 Dust, Clouds, and Eclipses on Mars Special Section: Ralph D. Lorenz1 , Mark T. Lemmon2 , Justin Maki3 , Donald Banfield4 , InSight at Mars 5,6 7 3 3 Aymeric Spiga
    [Show full text]
  • EGU2018-19456-1, 2018 EGU General Assembly 2018 © Author(S) 2018
    Geophysical Research Abstracts Vol. 20, EGU2018-19456-1, 2018 EGU General Assembly 2018 © Author(s) 2018. CC Attribution 4.0 license. DRAGONFLY: in situ exploration of Titan’s meteorology Scot Rafkin (1), Ralph Lorenz (2), Elizabeth Turtle (2), Jason Barnes (3), Melissa Trainer (4), Alice Le Gall (5), Juan Lora (6), Chris McKay (7), Claire Newman (8), Mark Panning (9), Kristin Sotzen (2), Tetsuya Tokano (10), Colin Wilson (11), and the Dragonfly Team (1) Southwest Research Institute, Boulder, CO, USA, (2) Johns Hopkins Applied Physics Lab., Laurel, MD, USA, (3) Univ. Idaho, Moscow, ID, USA, (4) NASA Goddard Space Flight Center, Greenbelt, MD, USA, (5) Laboratoire Atmosphères, Milieux, Observations Spatiales, Guyancourt, France, (6) Univ. California, Los Angeles, CA, USA, (7) NASA Ames Research Center, Moffett Field, CA, USA, (8) Aeolis Research, Pasadena, CA, USA, (9) Jet Propulsion Laboratory California Institute of Technology, Pasadena, CA, USA, (10) Inst. fur Geophysik und Meteorologie, Univ. Koln, Koln, Germany, (11) Oxford Univ., Oxford, UK Dragonfly is a rotorcraft lander mission currently in a Phase A study under NASA’s New Frontiers Program that would take advantage of Titan’s dense atmosphere and low gravity to visit a number of surface locations to study how far chemistry can progress in environments that provide key ingredients for life. This mission architecture also permits and demands investigation of Titan’s atmosphere. First, Dragonfly is a lander that will spend >2 Earth years on Titan’s surface, long enough to observe many diurnal cycles, atmospheric waves, and perhaps even some seasonal change. The DraGMet (Dragonfly Geophysics and Meteorology) instrument package includes measurement of wind speed and direction (using sensors on each of the four rotor pylons, to assure that one or more sensors are upwind of and thus unperturbed by the vehicle), temperature and pressure, and methane humidity.
    [Show full text]
  • Astrophysics
    Publications of the Astronomical Institute rais-mf—ii«o of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE IA U Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 1987 Publications of the Astronomical Institute of the Czechoslovak Academy of Sciences Publication No. 70 EUROPEAN REGIONAL ASTRONOMY MEETING OF THE I A U 10 Praha, Czechoslovakia August 24-29, 1987 ASTROPHYSICS Edited by PETR HARMANEC Proceedings, Vol. 5 1 987 CHIEF EDITOR OF THE PROCEEDINGS: LUBOS PEREK Astronomical Institute of the Czechoslovak Academy of Sciences 251 65 Ondrejov, Czechoslovakia TABLE OF CONTENTS Preface HI Invited discourse 3.-C. Pecker: Fran Tycho Brahe to Prague 1987: The Ever Changing Universe 3 lorlishdp on rapid variability of single, binary and Multiple stars A. Baglln: Time Scales and Physical Processes Involved (Review Paper) 13 Part 1 : Early-type stars P. Koubsfty: Evidence of Rapid Variability in Early-Type Stars (Review Paper) 25 NSV. Filtertdn, D.B. Gies, C.T. Bolton: The Incidence cf Absorption Line Profile Variability Among 33 the 0 Stars (Contributed Paper) R.K. Prinja, I.D. Howarth: Variability In the Stellar Wind of 68 Cygni - Not "Shells" or "Puffs", 39 but Streams (Contributed Paper) H. Hubert, B. Dagostlnoz, A.M. Hubert, M. Floquet: Short-Time Scale Variability In Some Be Stars 45 (Contributed Paper) G. talker, S. Yang, C. McDowall, G. Fahlman: Analysis of Nonradial Oscillations of Rapidly Rotating 49 Delta Scuti Stars (Contributed Paper) C. Sterken: The Variability of the Runaway Star S3 Arietis (Contributed Paper) S3 C. Blanco, A.
    [Show full text]
  • Titan Mare Explorer
    TiME Titan Mare Explorer Titan Mare Explorer (TiME): Proxemy Research First Exploration of an Extraterrestrial Sea Ellen Stofan TiME Science . Discovery of lakes and seas in Titan’s northern hemisphere confirmed the expectation that liquid hydrocarbons exist . Detection of the presence of ethane in Ontario Lacus near the South Pole (Brown et al., 2008) . 2 distinct types of features- lakes and seas, likely 10’s, >100 m deep . Post-Cassini, major questions will remain on the chemistry of sea liquids, their role in the overall methane cycle, the origin of sea basins, and seasonal processes and variability TiME Proprietary Information/Competition Sensitive Titan’s methane cycle • Titan’s methane cycle is analogous to Earth’s hydrologic cycle, with meteorological working fluid existing in condensed phase on surface and within crust, cycling through the surface atmosphere system and transporting mass and energy TiME Proprietary Information/Competition Sensitive TiME Science Target •Target: Ligeia Mare (78°N, 250°W) –One of the largest seas identified to date on Titan, surface area ~100,000 km2 –Backup target- Kraken Mare TiME Proprietary Information/Competition Sensitive TiME Science Team .PI: Ellen Stofan (Proxemy Research) .Co-Is: .Jonathan Lunine (Univ. of Az.) - Deputy PI .Ralph Lorenz (APL)- Project Scientist .Oded Aharonson (CalTech) .Beau Bierhaus (LM) .Ben Clark (SSI) .Caitlin Griffith (Univ. Arizona) .Ari-Matti Harri (FMI) .Erich Karkoschka (Univ. Arizona) .Randy Kirk (USGS) .Paul Mahaffy (Goddard) .Claire Newman (Ashima Research) .Mike Ravine (MSSS) .Melissa Trainer (GSFC) .Elizabeth Turtle (APL) .Hunter Waite (SWRI) .Margaret Yelland (Univ. Southampton) .John Zarnecki (Open University) TiME Proprietary Information/Competition Sensitive TiME Science Goals and Objectives .
    [Show full text]