Thesis Is Composed of Two Distinct Themes
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Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED -
With JWST: Science Justification and Observational Requirements
Observing Outer Planet Satellites (except Titan) with JWST: Science Justification and Observational Requirements Laszlo Keszthelyi1, Will Grundy2, John Stansberry3, Anand Sivaramakrishnan3, Deepashri Thatte3, Murthy Gudipati4, Constantine Tsang5, Alexandra Greenbaum6, Chima McGruder7 1U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001. ([email protected]) 2Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001. ([email protected]) 3Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218. ([email protected]; [email protected]; [email protected]) 4California Institute of Technology, Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109. ([email protected]) 5Southwest Research Institute, Department of Space Studies, 1050 Walnut St., Suite 300, Boulder, CO 80302. ([email protected]) 6 Department of Physics and Astronomy, 3400 N. Charles Street, Baltimore, MD 21218. ([email protected]) 7Department of Physics & Astronomy, 1408 Circle Drive, Knoxville, TN 37996. ([email protected]) ABSTRACT The James Webb Space Telescope (JWST) will allow observations with a unique combination of spectral, spatial, and temporal resolution for the study of outer planet satellites within our Solar System. We highlight the infrared spectroscopy of icy moons and temporal changes on geologically active satellites as two particularly valuable avenues of scientific inquiry. While some care must be taken to avoid saturation issues, JWST has observation modes that should provide excellent infrared data for such studies. KEYWORDS Solar System Astronomical Techniques 1. Introduction Starting in 2018, the James Webb Space Telescope (JWST) is expected to provide a groundbreaking new tool for astronomical observations, including planetary satellites as close as Phobos and Deimos. -
Revisiting the Sulfur-Water Chemical System in the Middle Atmosphere of Venus Wencheng Shao, Xi Zhang, Carver Bierson, Therese Encrenaz
Revisiting the Sulfur-Water Chemical System in the Middle Atmosphere of Venus Wencheng Shao, Xi Zhang, Carver Bierson, Therese Encrenaz To cite this version: Wencheng Shao, Xi Zhang, Carver Bierson, Therese Encrenaz. Revisiting the Sulfur-Water Chemi- cal System in the Middle Atmosphere of Venus. Journal of Geophysical Research. Planets, Wiley- Blackwell, 2020, 125 (8), pp.e06195. 10.1029/2019JE006195. hal-03250477 HAL Id: hal-03250477 https://hal.archives-ouvertes.fr/hal-03250477 Submitted on 11 Jun 2021 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. Copyright RESEARCH ARTICLE Revisiting the Sulfur‐Water Chemical System 10.1029/2019JE006195 in the Middle Atmosphere of Venus Key Points: Wencheng D. Shao1 , Xi Zhang1 , Carver J. Bierson1 , and Therese Encrenaz2 • We found that there is no bifurcation behavior in the 1Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA, USA, 2LESIA, Observatoire de sulfur‐water chemical system as previously claimed Paris, PSL University, CNRS, Sorbonne University, University Sorbonne Paris City, Meudon, France • The observed SO2‐H2O anticorrelation can be explained by the sulfur‐water chemistry with Abstract Sulfur‐water chemistry plays an important role in the middle atmosphere of Venus. -
Mass of the Kuiper Belt · 9Th Planet PACS 95.10.Ce · 96.12.De · 96.12.Fe · 96.20.-N · 96.30.-T
Celestial Mechanics and Dynamical Astronomy manuscript No. (will be inserted by the editor) Mass of the Kuiper Belt E. V. Pitjeva · N. P. Pitjev Received: 13 December 2017 / Accepted: 24 August 2018 The final publication ia available at Springer via http://doi.org/10.1007/s10569-018-9853-5 Abstract The Kuiper belt includes tens of thousands of large bodies and millions of smaller objects. The main part of the belt objects is located in the annular zone between 39.4 au and 47.8 au from the Sun, the boundaries correspond to the average distances for orbital resonances 3:2 and 2:1 with the motion of Neptune. One-dimensional, two-dimensional, and discrete rings to model the total gravitational attraction of numerous belt objects are consid- ered. The discrete rotating model most correctly reflects the real interaction of bodies in the Solar system. The masses of the model rings were determined within EPM2017—the new version of ephemerides of planets and the Moon at IAA RAS—by fitting spacecraft ranging observations. The total mass of the Kuiper belt was calculated as the sum of the masses of the 31 largest trans-neptunian objects directly included in the simultaneous integration and the estimated mass of the model of the discrete ring of TNO. The total mass −2 is (1.97 ± 0.30) · 10 m⊕. The gravitational influence of the Kuiper belt on Jupiter, Saturn, Uranus and Neptune exceeds at times the attraction of the hypothetical 9th planet with a mass of ∼ 10 m⊕ at the distances assumed for it. -
Arxiv:2012.11628V3 [Astro-Ph.EP] 26 Jan 2021
manuscript submitted to JGR: Planets The Fundamental Connections Between the Solar System and Exoplanetary Science Stephen R. Kane1, Giada N. Arney2, Paul K. Byrne3, Paul A. Dalba1∗, Steven J. Desch4, Jonti Horner5, Noam R. Izenberg6, Kathleen E. Mandt6, Victoria S. Meadows7, Lynnae C. Quick8 1Department of Earth and Planetary Sciences, University of California, Riverside, CA 92521, USA 2Planetary Systems Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 3Planetary Research Group, Department of Marine, Earth, and Atmospheric Sciences, North Carolina State University, Raleigh, NC 27695, USA 4School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA 5Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD 4350, Australia 6Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA 7Department of Astronomy, University of Washington, Seattle, WA 98195, USA 8Planetary Geology, Geophysics and Geochemistry Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Key Points: • Exoplanetary science is rapidly expanding towards characterization of atmospheres and interiors. • Planetary science has similarly undergone rapid expansion of understanding plan- etary processes and evolution. • Effective studies of exoplanets require models and in-situ data derived from plan- etary science observations and exploration. arXiv:2012.11628v4 [astro-ph.EP] 8 Aug 2021 ∗NSF Astronomy and Astrophysics Postdoctoral Fellow Corresponding author: Stephen R. Kane, [email protected] {1{ manuscript submitted to JGR: Planets Abstract Over the past several decades, thousands of planets have been discovered outside of our Solar System. These planets exhibit enormous diversity, and their large numbers provide a statistical opportunity to place our Solar System within the broader context of planetary structure, atmospheres, architectures, formation, and evolution. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
UC Santa Cruz UC Santa Cruz Electronic Theses and Dissertations
UC Santa Cruz UC Santa Cruz Electronic Theses and Dissertations Title The chemical structure of Venus's atmosphere and interior evolution of Kuiper belt objects Permalink https://escholarship.org/uc/item/3tt926w1 Author Bierson, Carver Jay Publication Date 2020 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California UNIVERSITY OF CALIFORNIA SANTA CRUZ THE CHEMICAL STRUCTURE OF VENUS'S ATMOSPHERE AND INTERIOR EVOLUTION OF KUIPER BELT OBJECTS A dissertation submitted in partial satisfaction of the requirements for the degree of DOCTOR OF PHILOSOPHY in EARTH SCIENCE by Carver Jay Bierson June 2020 The Dissertation of Carver Jay Bierson is approved: Professor Francis Nimmo, Chair Professor Xi Zhang Professor Nicole Feldl Dr. Kevin Zahnle Quentin Williams Acting Vice Provost and Dean of Graduate Studies Copyright c by Carver Jay Bierson 2020 Table of Contents List of Figures v List of Tables ix Abstract xi Dedication xiii Acknowledgments xiv 1 Introduction 1 2 Chemical cycling in the Venusian atmosphere: A full photo-chemical model from the surface to 110 km 4 2.1 Introduction . .5 2.1.1 Overview of Chemical cycles . .6 2.1.2 Previous models . .9 2.2 Model Description . 11 2.2.1 Boundary conditions . 15 2.2.2 Modifications to our nominal case . 16 2.3 Results . 17 2.3.1 SOx .................................. 17 2.3.2 CO and OCS . 23 2.3.3 Ox ................................... 30 2.3.4 Chlorides . 31 2.3.5 Other Species . 34 2.4 Summary . 35 3 Implications of the Observed Pluto-Charon Density Contrast 40 3.1 Introduction . -
Gordon Taylor
Journal for Occultation Astronomy 2 0 1 6 – 04 Iridescent clouds AndreasTegtmeier during the annular eclipse 2016 Sept. 1 © IN THIS ISSUE: l Gordon Taylor An astronomical autobiography l ESOP XXXV University of Guildford Surrey, England l Beyond Jupiter The world of distant minor planets (120347) Salacia l Baily’s Beads Observation during the annular eclipse 2016 Sept. 1 l Leap Seconds Journal for Occultation Astronomy · Sept.-Nov. 2016 1 Dear reader, Writing articles for JOA: The rules below should be regarded while writing an article; using 2016 was a year of many highlights in occultation astronomy. The them will greatly facilitate the production and layout of ON! GAIA catalogue appeared with its first release. Our 20 inch portable If your article does not conform to these rules, please correct it. occultation telescope “M2” served its first scientific observation. There are 3 different possibilities for submitting articles: Once more an occultation by Pluto and Chariklo with its rings could n be observed to mention only the most remarkable events. pdf-articles (must be editable – these can be converted) n unformatted Word *.doc-files containing pictures/graphs or But now in 2017 the story will continue. Everybody is encouraged their names (marked red: <figure_01>) at the desired position(s) to record lightcurves of asteroidal occultations in order to improve n the mapping of their three-dimensional shapes. The observation of *.txt-files must contain at the desired position the name of each graph/picture mutual events of asteroids and their satellite(s) gives unprecedented insights, as for Kalliope in the first months of 2017. -
2005 Astronomy Magazine Index
2005 Astronomy Magazine Index Subject index flyby of Titan, 2:72–77 Einstein, Albert, 2:30–53 Cassiopeia (constellation), 11:20 See also relativity, theory of Numbers Cassiopeia A (supernova), stellar handwritten manuscript found, 3C 58 (star remnant), pulsar in, 3:24 remains inside, 9:22 12:26 3-inch telescopes, 12:84–89 Cat's Eye Nebula, dying star in, 1:24 Einstein rings, 11:27 87 Sylvia (asteroid), two moons of, Celestron's ExploraScope telescope, Elysium Planitia (on Mars), 5:30 12:33 2:92–94 Enceladus (Saturn's moon), 11:32 2003 UB313, 10:27, 11:68–69 Cepheid luminosities, 1:72 atmosphere of water vapor, 6:22 2004, review of, 1:31–40 Chasma Boreale (on Mars), 7:28 Cassini flyby, 7:62–65, 10:32 25143 (asteroid), 11:27 chonrites, and gamma-ray bursts, 5:30 Eros (asteroid), 11:28 coins, celestial images on, 3:72–73 Eso Chasma (on Mars), 7:28 color filters, 6:67 Espenak, Fred, 2:86–89 A Comet Hale-Bopp, 7:76–79 extrasolar comets, 9:30 Aeolis (on Mars), 3:28 comets extrasolar planets Alba Patera (Martian volcano), 2:28 from beyond solar system, 12:82 first image of, 4:20, 8:26 Aldrin, Buzz, 5:40–45 dust trails of, 12:72–73 first light from, who captured, 7:30 Altair (star), 9:20 evolution of, 9:46–51 newly discovered low-mass planets, Amalthea (Jupiter's moon), 9:28 extrasolar, 9:30 1:68–71 amateur telescopes. See telescopes, Conselice, Christopher, 1:20 smallest, 9:26 amateur constellations whether have diamond layers, 5:26 Andromeda Galaxy (M31), 10:84–89 See also names of specific extraterrestrial life, 4:28–34 disk of stars surrounding, 7:28 constellations eyepieces, telescope. -
The Thermal and Orbital Evolution of Enceladus: Observational Constraints and Models
The thermal and orbital evolution of Enceladus: observational constraints and models Francis Nimmo UCSC Amy C. Barr PSI Marie Behounkovˇ a´ Charles University William B. McKinnon Washington University Enceladus possesses a global subsurface ocean beneath an ice shell a few tens of km thick, and is observed to be losing heat at a rate of ∼10 GW from its south polar region. Two major puzzles are the source of the observed heat, and how the ocean could have been maintained. Tidal dissipation in Enceladus is ultimately controlled by the rate of dissipation within Saturn, parameterized by the factor Qp.A Qp of about 2,000 is indicated by astrometric measurements and generates an equilibrium heating rate at Enceladus sufficient to explain the observed heat and maintain an ocean indefinitely if the ice shell is conductive. If constant, this Qp would indicate an age for Enceladus much less than that of the solar system. An alternative, however, termed the “resonance-locking” scenario, is that the effective Qp is time-variable such that the heating rate is almost constant over geological time. This scenario can explain the long-term survival of the ocean and the present-day heat flux without requiring Enceladus to have formed recently. 1. INTRODUCTION details of how this actually works are not well understood. A particularly difficult aspect of satellite evolution is that Enceladus, despite its limited size, is one of the most their thermal and orbital evolution are often intimately cou- surprising bodies in the solar system with a south polar ter- pled. This is because the amount of tidal heating depends rain (SPT) containing localized active tectonics, remarkable on the satellite’s mechanical properties, many of which geysers connected to four prominent fracture sets (the “tiger are temperature-dependent. -
AST-2017-1693-Ver9-Rushby 4P 469..480
Long-Term Planetary Habitability and the Carbonate-Silicate Cycle Andrew J. Rushby,1,2 Martin Johnson,2,3 Benjamin J.W. Mills,4 Andrew J. Watson,5 and Mark W. Claire6,7,8 Abstract The potential habitability of an exoplanet is traditionally assessed by determining whether its orbit falls within the circumstellar ‘‘habitable zone’’ of its star, defined as the distance at which water could be liquid on the surface of a planet (Kopparapu et al., 2013). Traditionally, these limits are determined by radiative-convective climate models, which are used to predict surface temperatures at user-specified levels of greenhouse gases. This approach ignores the vital question of the (bio)geochemical plausibility of the proposed chemical abundances. Carbon dioxide is the most important greenhouse gas in Earth’s atmosphere in terms of regulating planetary temperature, with the long- term concentration controlled by the balance between volcanic outgassing and the sequestration of CO2 via chemical weathering and sedimentation, as modulated by ocean chemistry, circulation, and biological (microbial) productivity. We developed a model that incorporates key aspects of Earth’s short- and long-term biogeochemical carbon cycle to explore the potential changes in the CO2 greenhouse due to variance in planet size and stellar insolation. We find that proposed changes in global topography, tectonics, and the hydrological cycle on larger planets result in proportionally greater surface temperatures for a given incident flux. For planets between 0.5 and 2 R4, the effect of these changes results in average global surface temperature deviations of up to 20 K, which suggests that these relationships must be considered in future studies of planetary habitability. -
Mercury Biogeochemical Cycling: a Synthesis of Recent Scientific Advances
Science of the Total Environment 737 (2020) 139619 Contents lists available at ScienceDirect Science of the Total Environment journal homepage: www.elsevier.com/locate/scitotenv Mercury biogeochemical cycling: A synthesis of recent scientific advances Mae Sexauer Gustin a,⁎, Michael S. Bank b,c, Kevin Bishop d, Katlin Bowman e,f, Brian Branfireun g, John Chételat h, Chris S. Eckley i, Chad R. Hammerschmidt j, Carl Lamborg f, Seth Lyman k, Antonio Martínez-Cortizas l, Jonas Sommar m, Martin Tsz-Ki Tsui n, Tong Zhang o a Department of Natural Resources and Environmental Science, University of Nevada, Reno, NV 89439, USA b Department of Contaminants and Biohazards, Institute of Marine Research, Bergen, Norway c Department of Environmental Conservation, University of Massachusetts, Amherst, MA 01255, USA d Department of Aquatic Sciences and Assessment, Swedish University of Agricultural Sciences, Box 7050, 75007 Uppsala, Sweden e Moss Landing Marine Laboratories, 8272 Moss Landing Road, Moss Landing, CA 95039, USA f University of California Santa Cruz, Ocean Sciences Department, 1156 High Street, Santa Cruz, CA 95064, USA g Department of Biology and Centre for Environment and Sustainability, Western University, London, Canada h Environment and Climate Change Canada, National Wildlife Research Centre, 1125 Colonel By Drive, Ottawa, ON K1A 0H3, Canada i U.S. Environmental Protection Agency, Region-10, 1200 6th Ave, Seattle, WA 98101, USA j Wright State University, Department of Earth and Environmental Sciences, 3640 Colonel Glenn Highway, Dayton,