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Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 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. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes. -
Final Report for a Robotic Exploration Mission to Mars and Phobos Argos
NASA-CR-197168 NASw-4435 /'/F/ 4 '_/e'7 t'/-q 1- Final Report for a Robotic Exploration Mission to Mars and Phobos PROJECT AENEAS Response to RFP Number ASE274L.0893 o r,4 u_ 4" submitted to: I ,-- ,0 U i'_ C_ e" 0 Z _ 0 Dr. George Botbyl The University of Texas at Austin Department of Aerospace Engineering and Engineering Mechanics Austin, Texas 78712 Z cn _. submitted by: 0 cO_ 0 Argos Space Endeavours 29 November 1993 zxI_f _rOos 8Face _.aea_ours _roJect Aeneas CDestBn _"eam Fall 1993 Chief Executive Officer Justin H. Kerr Chief Engineer Erin Defoss6 Chief Administrator Quang Ho Engineers Emisto Barriga Grant Davis Steve McCourt Matt Smith Aeneas Project Preliminary Design of a Robotic Exploration Mission to Mars and Phobos Approved: Justin H. Kerr CEO, Argos Space Endeavours Approved: Erin Defoss6 Chief Engineer, Argos Space Endeavours Approved: Quang Ho Administrative Officer, Argos Space Endeavours Argos 8pace q .aca ours University of Texas at Austin Department of Aerospace Engineering and Engineering Mechanics November 1993 Acknowledgments Argos Space Endeavours would like to thank all personnel at The University and in industry who made Project Aeneas possible. This project was conducted with the support of the NASA/USRA Advanced Design Program. Argos Space Endeavours wholeheartedly thanks the following faculty, staff, and students from the University of Texas at Austin: Dr. Wallace Fowler, Dr. Ronald Stearman, Dr. John Lundberg, Professor Richard Drury, Dr. David Dolling, Ms. Kelly Spears, Mr. Elfego Piton, Mr. Tony Economopoulos, and Mr. David Garza. The support of Project Aeneas from the aerospace industry was overwhelming. -
Phobos State of Knowledge and Rationales for Future Exploration
Phobos/Deimos State of Knowledge in Preparation for Future Exploration Julie Castillo-Rogez Laboratory for Frozen Astromaterials, PI NIAC for Hybrid Rovers/Hoppers, Study Scientist Jet Propulsion Laboratory, California Institute of Technology Initial Phobos/Deimos DRM Meeting for HAT Outline Introduction Science at Phobos Deimos Human Exploration Considerations Outline Introduction Science at Phobos Deimos Human Exploration Considerations Scope • Characterize Phobos/Deimos environment - Soil properties – mechanical and chemical - Surface dynamics - Subsurface properties (e.g., caves, regolith thickness) - Hazards – Radiations, topography, dust, electrostatic charging • Identify potential landing sites - Hazards – topography, surface dynamics - Vantage point wrt Mars - Scientific interest Moons Properties Phobos Deimos Shape (km) 26.8 × 22.4 × 18.4 15 × 12.2 × 10.4 Density (kg/m3) 1876 1471 Surface Gravity (Equator) µg 190-860 390 Escape Velocity (m/s) 11.3 5.6 SMA (km) 9,377 23,460 Eccentricity 0.015 1 0.000 2 Rotation Period (hr) 7h39.2 30h18 Forced Libration in Longitude 1.24±0.15 ?? (deg.) Orbital Period (hr) Synchronous Synchronous Equatorial Rotation Velocity 11.0 1.6 (km/h) – Longest axis Surface Temperature (K) 150-300 233 Outline Introduction Science at Phobos Deimos Human Exploration Considerations Key Science • Mysterious origin is endless subject of discussion – Remnant planetesimal vs. captured asteroid vs. Mars ejectas – Brings constraints on Mars’ early history and/or Solar system • Likely to have accumulated material from -
Human Spaceflight: Phobos Base
2017 AIAA Student Design Competition HUMAN SPACEFLIGHT: PHOBOS BASE Timothy Bishop Victor Kitmanyen Thomas Lagarde Zachary Taylor Faculty Advisor: Olga Bannova, Ph.D. Sasakawa International Center for Space Architecture (SICSA) Cullen College of Engineering, University of Houston Houston, Texas, USA ~ 2 ~ Copyright © 2017 by Timothy Bishop, Victor Kitmanyen, Thomas Lagarde & Zachary Taylor. All Rights Reserved. Published with express permission, by the American Institute of Aeronautics and Astronautics, Inc. ~ 3 ~ Signature Page Timothy Bishop Project Manager AIAA #: 677333 Victor Kitmanyen Microgravity Countermeasures Architect AIAA #: 819885 Zachary Taylor Space Architect AIAA #: 819283 Thomas Lagarde RECLSS Architect AIAA #: 819864 Dr. Olga Bannova Faculty & Project Advisor Copyright © 2017 by Timothy Bishop, Victor Kitmanyen, Thomas Lagarde & Zachary Taylor. All Rights Reserved. Published with express permission, by the American Institute of Aeronautics and Astronautics, Inc. ~ 4 ~ Table of Contents LIST OF FIGURES ___________________________________________________________________________ 6 ACRONYMS _________________________________________________________________________________ 8 1.0 ABSTRACT _______________________________________________________________________________ 9 2.0 PROJECT INTRODUCTION ______________________________________________________________ 10 3.0 REQUIREMENTS: ANALYSIS AND INTERPRETATION ____________________________________ 11 3.1 SITE ___________________________________________________________________________________ -
GURPS Classic Mars
MARS The Red Planet Written by James L. Cambias Additional material by Kenneth Peters Edited by Scott Haring Cover art by Christopher Shy Illustrated by Paul Daly GURPS System Design ! Steve Jackson GURPS Line Editor ! Sean Punch Managing Editor ! Andrew Hackard Project Administrator ! Monique Chapman Production Manager ! Heather Oliver Creative Director ! Philip Reed Production Artist ! Heather Oliver Production Assistance ! Alex Fernandez Page Designer ! Jack Elmy Print Buyer ! Monica Stephens Sales Manager ! Ross Jepson Errata Coordinator ! Andy Vetromile Lead Playtester: Steph Pennington Assistant Lead Playtester: Devin L. Ganger Playtesters: Frederick Bracken, Nelson Cunnington, Jeremiah Genest, Anthony Jackson, M.A. Lloyd, David Morgan-Mar, Kenneth Peters, Bill Stoddard, and Constantine Thomas Special Thanks to: Dr. Diane A. Kelly, Dr. Geoffrey A. Landis, Richard Wagner, and Dr. Keith Watt. And thanks to everyone who provided information or commentary. GURPS, Warehouse 23, and the all-seeing pyramid are registered trademarks of Steve Jackson Games Incorporated. Pyramid and the names of all products published by Steve Jackson Games Incorporated are registered trademarks or trademarks of Steve Jackson Games Incorporated, or used under license. GURPS Mars is copyright © 2002 by Steve Jackson Games Incorporated. All rights reserved. Some art copyright www.arttoday.com. Some art courtesy of NASA/JPL/Caltech. Printed in the USA. ISBN 1-55634-534-8 1 2 3 4 5 6 7 8 9 10 STEVE JACKSON GAMES CONTENTS Introduction . 4 Looking for Life . 30 Fortean Mars . 46 Invaders from Earth. 30 Velikovskian Mars . 47 About the Author . 4 The Martian Meteorite. 30 Capricorn One . 47 1. Mars Observed . 5 GETTING TO MARS . -
Mars Orbiter and Lander (ESA)
So much nonsense has been written about the planet … that it is easy to forget that Mars is still an object of serious scientific investigation. Canadian astronomer Peter M. Millman, in “Is There Vegetation on Mars,” The Sky, 3, 10–11 (1939) Tentative Course outline • Today: Intro to Mars, Early discoveries about Mars (Chapters 1-4) • Oct 17: Canals on Mars, Water on Mars (Chapters 5-8) • Oct 24: Lichens on Mars (Chapter 9) • Oct 31: Viking mission (Chapter 10) • Nov 7: ALH 84001 (Chapter 11) • Nov 14: Methane on Mars (Chapters 12-15) Earth and Mars Basic Facts Earth Mars • 93 million miles from • 142 million miles from sun sun • Diameter: 4,212 miles • Diameter: 7,918 miles (53% of Earth) • Orbit: 365.25 days • Mass: 10.7% of Earth • Solid surface • Orbit: 687 days • Thin atmosphere • Solid surface • Thin atmosphere • 1 big moon • 2 little moons Basic Facts about Earth and Solar System • Sun and planets formed at same time The Nebular Hypothesis Immanuel Pierre Kant Laplace 1755 1796 sun (center) and planets (in disk) form at same time out of rotating cloud that collapses under the force of gravity An ALMA image of the star HD 163296 and its protoplanetary disk as seen in dust. New observations suggested that two planets, each about the size of Saturn, are in orbit around the star. These planets, which are not yet fully formed, revealed themselves in the dual imprint they left in both the dust and the gas portions of the star's protoplanetary disk. Credit: ALMA (ESO/NAOJ/NRAO), Andrea Isella, B. -
The Age of Phobos and Its Largest Crater, Stickney
Planetary and Space Science 102 (2014) 152–163 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss The age of Phobos and its largest crater, Stickney N. Schmedemann a,n, G.G. Michael a, B.A. Ivanov b, J.B. Murray c, G. Neukum a a Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany b Institute of Dynamics of Geospheres, Moscow, Russia c Department of Earth Sciences, Open University, Milton Keynes, UK article info abstract Article history: We derived crater production functions and chronology functions of Phobos for two scenarios, which Received 15 December 2012 likely represent the end-members of its dynamical evolution. Case A assumes that Phobos has been in its Received in revised form current orbit about Mars since its formation. Case B assumes a recent capture of Phobos and the impact 25 February 2014 history of an average Main Belt Asteroid. We determined the age of an average surface to the west of the Accepted 16 April 2014 Stickney crater and of the interior of the Stickney crater. The results indicate (i) the formation or major Available online 26 April 2014 collision of Phobos about 4.3 Ga (Case A) or 3.5 Ga (Case B) ago, (ii) the Stickney crater is about 4.2 Ga Keywords: (Case A) or 2.6 Ga (Case B) old and (iii) grooves probably formed between 3.1 and 3.8 Ga (Case A) or 44 Phobos and 340 Ma (Case B). Thus, Stickney seems to be older than the investigated grooves on Phobos. -
(PHLOTE) NASA Advanced Innovative Concepts Phase 1 Study
Phobos L1 Operational Tether Experiment NASA Advanced Innovative Phase I Study Report Revision: 1.0 Concepts Program Document Date: 2/2/201 8 Page 1 of 91 Phase I Study Report For The Phobos L1 Operational Tether Experiment (PHLOTE) NASA Advanced Innovative Concept s Phase 1 Study Phobos L1 Operational Tether Experiment NASA Advanced Innovative Phase I Study Report Revision: 1.0 Concepts Program Document Date: 2/2/201 8 Page 2 of 91 FINAL REPORT NASA Innovative Advanced Concepts (NIAC) PHLOTE: Phobos Lagrange -1 Operational Tether Experiment Principal Investigator: Kevin Kempton (NASA Langley Research Center) Co-Investigators: Jerome Pearson, Eugene Levin, Joe Carroll (STAR Inc.) Farzin Amzajerdian, Mia Siochi (NASA Langley Research Center) PHLOTE Interns: Madeline Pomicter (University of Vermont), Zachary Wells (Virginia Polytech Institute and State University), Amber Dubill (Rochester Institute of Technology), Haley Uline (Miami University), Stephen Richards (Old Dominion University) Graphics Support from the Clouds Architecture Office (Clouds AO) Febru ary 2018 Phobos L1 Operational Tether Experiment NASA Advanced Innovative Phase I Study Report Revision: 1.0 Concepts Program Document Date: 2/2/201 8 Page 3 of 91 Table of Contents INTRODUCTION ....................................................................................................................................................... 5 REFERENCES ........................................................................................................................................................... -
Planets Solar System Paper Contents
Planets Solar system paper Contents 1 Jupiter 1 1.1 Structure ............................................... 1 1.1.1 Composition ......................................... 1 1.1.2 Mass and size ......................................... 2 1.1.3 Internal structure ....................................... 2 1.2 Atmosphere .............................................. 3 1.2.1 Cloud layers ......................................... 3 1.2.2 Great Red Spot and other vortices .............................. 4 1.3 Planetary rings ............................................ 4 1.4 Magnetosphere ............................................ 5 1.5 Orbit and rotation ........................................... 5 1.6 Observation .............................................. 6 1.7 Research and exploration ....................................... 6 1.7.1 Pre-telescopic research .................................... 6 1.7.2 Ground-based telescope research ............................... 7 1.7.3 Radiotelescope research ................................... 8 1.7.4 Exploration with space probes ................................ 8 1.8 Moons ................................................. 9 1.8.1 Galilean moons ........................................ 10 1.8.2 Classification of moons .................................... 10 1.9 Interaction with the Solar System ................................... 10 1.9.1 Impacts ............................................ 11 1.10 Possibility of life ........................................... 12 1.11 Mythology ............................................. -
Arxiv:1705.02260V1
Meteorites from Phobos and Deimos at Earth? Accepted by Planetary and Space Science P. Wiegerta,b, M. A. Galiazzoa,b,c aDepartment of Physics and Astronomy, The University of Western Ontario, London, Ontario, N6A 3K7, Canada bCentre for Planetary Science and Exploration (CPSX), London, Ontario, N6A 3K7, Canada cInstitute of Astrophysics, University of Vienna, Turkenschanzstr. 17, A-1180 Vienna, Austria Abstract We examine the conditions under which material from the martian moons Phobos and Deimos could reach our planet in the form of meteorites. We find that the necessary ejection speeds from these moons (900 and 600 m/s for Phobos and Deimos respectively) are much smaller than from Mars’ surface (5000 m/s). These speeds are below typical impact speeds for asteroids and comets (10-40 km/s) at Mars’ orbit, and we conclude that the delivery of meteorites from Phobos and Deimos to the Earth can occur. Keywords: Mars, Phobos, Deimos, Earth, meteorite 1. Introduction Meteorites are solid interplanetary material that survives its passage through the Earth’s atmo- sphere and arrives at the ground. Most meteorites originate from minor bodies, but a few arrive from planetary bodies. The interchange of material between the Mars and Earth is now well-established, both from the point of view of the ejection of material from the martian surface (Head et al., 2002), as well as of the orbital dynamics of Mars-Earth transfer (Gladman et al., 1996). At this writing fifty meteorites from Mars are recognized among the world’s meteorite collections (The Meteorit- ical Bulletin Database1). Here we examine one remaining open question in this field, and that is whether material might arrive at the Earth from the martian satellites. -
Asteroid Redirect Mission (ARM) Formulation Assessment and Support Team (FAST) Final Report Draft for Public Comment
This document is a NASA working document and is subject to further revision. This document been reviewed for release to the public and is not export controlled. Asteroid Redirect Mission (ARM) Formulation Assessment and Support Team (FAST) Final Report Draft for Public Comment November 23, 2015 This document is a NASA working document and is subject to further revision. This document been reviewed for release to the public and is not export controlled. This Page left Intentionally Blank 1 This document is a NASA working document and is subject to further revision. This document been reviewed for release to the public and is not export controlled. Contents Executive Summary ....................................................................................................................................... 3 FAST Overview ............................................................................................................................................ 13 Purpose ................................................................................................................................................... 13 Asteroid Redirect Mission Background ................................................................................................... 13 Study Request .......................................................................................................................................... 15 Membership ........................................................................................................................................... -
(Hirise) During MRO's Primary Science Phase (PSP) Alfred S
Icarus 205 (2010) 2-37 Contents lists available at ScienceDirect Icarus ELSEVIER journal homepage: www.elsevier.com/locate/icarus The High Resolution Imaging Science Experiment (HiRISE) during MRO's Primary Science Phase (PSP) Alfred S. McEwen3-*, Maria E. Banks3, Nicole Baugh3, Kris Beckerb, Aaron Boyd3, James W. Bergstromc, Ross A. Beyerd, Edward Bortolinic, Nathan T. Bridges6, Shane Byrne3, Bradford Castalia3, Frank C. Chuangf, Larry S. Grumpier ^, Ingrid Daubar3, Alix K. Davatzesh, Donald G. Deardorffd, Alaina Dejong3, W. Alan Delamere1, Eldar Noe Dobreae, Colin M. Dundas3, Eric M. Eliason3, Yisrael Espinoza3, Audrie Fennema3, Kathryn E. Fishbaughj, Terry Forrester3, Paul E. Geisslerb, John A. GrantJ, Jennifer L Griffes k, John P. Grotzingerk, Virginia C. Gulickd, Candice J. Hansen6, Kenneth E. Herkenhoffb, Rodney Heyd 3, Windy L Jaeger b, Dean Jones3, Bob Kanefsky d, Laszlo Keszthelyib, Robert King 3, Randolph L Kirkb, Kelly J. Kolb3, Jeffrey Lascoc, Alexandra Lefort1, Richard Leis3, Kevin W. Lewis k, Sara Martinez-Alonsom, Sarah Mattson3, Guy McArthur3, Michael T. Mellon•, Joannah M. Metzk, Moses P. Milazzob, Ralph E. Milliken6, Tahirih Motazedian3, Chris H. Okubob, Albert Ortiz3, Andrea J. Philippoff3, Joseph Plassmann3, Anjani Polit3, Patrick S. Russell1, Christian Schaller3, Mindi L Searlsm, Timothy Spriggs3, Steven W. Squyres", Steven Tarrc, Nicolas Thomas1, Bradley J. Thomson6,0, Livio L. Tornabene3, Charlie Van Houtenc, Circe Verbab, Catherine M. Weitzf, James J. Wray n "Lunar and Planetary Lab, University of Arizona, Tucson, AZ 85721, USA bU.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001, USA cBall Aerospace & Technologies Corp., 1600 Commerce St., Boulder, CO 80301, USA dNASA Ames Research Center and SETI Institute, Moffett Field, CA 94035, USA eJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA 'Planetary Science Institute, 1700 E.