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Selection of the Insight Landing Site M. Golombek1, D. Kipp1, N
Manuscript Click here to download Manuscript InSight Landing Site Paper v9 Rev.docx Click here to view linked References Selection of the InSight Landing Site M. Golombek1, D. Kipp1, N. Warner1,2, I. J. Daubar1, R. Fergason3, R. Kirk3, R. Beyer4, A. Huertas1, S. Piqueux1, N. E. Putzig5, B. A. Campbell6, G. A. Morgan6, C. Charalambous7, W. T. Pike7, K. Gwinner8, F. Calef1, D. Kass1, M. Mischna1, J. Ashley1, C. Bloom1,9, N. Wigton1,10, T. Hare3, C. Schwartz1, H. Gengl1, L. Redmond1,11, M. Trautman1,12, J. Sweeney2, C. Grima11, I. B. Smith5, E. Sklyanskiy1, M. Lisano1, J. Benardino1, S. Smrekar1, P. Lognonné13, W. B. Banerdt1 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 2State University of New York at Geneseo, Department of Geological Sciences, 1 College Circle, Geneseo, NY 14454 3Astrogeology Science Center, U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001 4Sagan Center at the SETI Institute and NASA Ames Research Center, Moffett Field, CA 94035 5Southwest Research Institute, Boulder, CO 80302; Now at Planetary Science Institute, Lakewood, CO 80401 6Smithsonian Institution, NASM CEPS, 6th at Independence SW, Washington, DC, 20560 7Department of Electrical and Electronic Engineering, Imperial College, South Kensington Campus, London 8German Aerospace Center (DLR), Institute of Planetary Research, 12489 Berlin, Germany 9Occidental College, Los Angeles, CA; Now at Central Washington University, Ellensburg, WA 98926 10Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996 11Institute for Geophysics, University of Texas, Austin, TX 78712 12MS GIS Program, University of Redlands, 1200 E. Colton Ave., Redlands, CA 92373-0999 13Institut Physique du Globe de Paris, Paris Cité, Université Paris Sorbonne, France Diderot Submitted to Space Science Reviews, Special InSight Issue v. -
Magnetic Planets and Magnetic Planets and How Mars Lost Its
Magnetic Planets and How Mars Lost Its Atmosphere Bob Lin Physics Department & Space Sciences Laboratory Universityyf of Calif ornia, Berkeley Also (visiting) School of Space Research Kyung Hee University, Korea Thanks to the MGS, MAVEN, and LP teams Earth’s Magnetic Field The Earth’s Magnetosphere Explorer 35 (1967) Lunar Shadowing Apollo 15 Mission -1971 Lunar Rover -> <- Jim Arnold's Gamma-ray Spectrometer <- Apollo 15 Subsatellite -> <= SIM (Scientific Instrument Module) Lunar Shadowing <= Downward electrons <= Upward electrons <= Ratio of Upward to DdltDownward electrons Electron Reflection Electron Trajectory Converging Magnetic Fields Secondary Electron ---- ---- - dv||RemotelydU SensingdB Surface MagneticB Fields by m + e + μ = 0⇒sin 2 α = LP []1- eΔU E Planetary Electron Reflection Magnetometryc (PERM) dt ds ds BSurf Apollo 15 & 16 Subsatellites Electron Reflectometry OneHowever, of the the great Apollo surprises 15 & 16 from Subsatellite Apollo was magnetic the discovery data set of paleomagneticis very sparse and fields confined in the lunar within crust 35 degrees. Their existence of the suggestsequator. Attempts that magnetic to correlate fields atsurface the Moon magnetic were muchfields with strongerspecific geologic in the past features than they were are largely today. unsuccessful. Mars Observer (1992-3) – disappeared 3 days before Mars orbit insertion Mars Global Surveyy(or (MGS) 1996-2006 MGS Mag/ER team Current state of knowledge • Very strong crustal fields measured from orbit: – Discovered by MGS: ~10 times stronger -
MSS/1: Single‐Station and Single‐Event Marsquake Inversion
RESEARCH ARTICLE MSS/1: Single‐Station and Single‐Event 10.1029/2020EA001118 Marsquake Inversion Special Section: Mélanie Drilleau1,2 , Éric Beucler3 , Philippe Lognonné1 , Mark P. Panning4 , InSight at Mars 5 4 6,7 8 Brigitte Knapmeyer‐Endrun , W. Bruce Banerdt , Caroline Beghein , Savas Ceylan , Martin van Driel8 , Rakshit Joshi9 , Taichi Kawamura1, Amir Khan8,10 , Key Points: Sabrina Menina1 , Attilio Rivoldini11 , Henri Samuel1 , Simon Stähler8 , Haotian Xu6 , • In the framework on the InSight 3 8 8 1 12 mission, a synthetic seismogram Mickaël Bonnin , John Clinton , Domenico Giardini , Balthasar Kenda , Vedran Lekic , 3 2 13 4 using a 3‐D crust and a 1‐D velocity Antoine Mocquet , Naomi Murdoch , Martin Schimmel , Suzanne E. Smrekar , model below is proposed Éléonore Stutzmann1 , Benoit Tauzin14,15 , and Saikiran Tharimena4 • This signal is used to present inversion methods, relying on 1Institut de Physique du Globe de Paris, Sorbonne Paris Cité, CNRS F‐7500511, Université Paris Diderot, Paris, France, different parameterizations, to 2ISAE‐SUPAERO, Toulouse University, Toulouse, France, 3Laboratoire de Planétologie et de Géodynamique, Université constrain the 1‐D structure of Mars 4 • The results demonstrate the de Nantes, Université d'Angers, Nantes, France, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, feasibility of the strategy to retrieve CA, USA, 5Bensberg Observatory, University of Cologne, Cologne, Germany, 6Department of Earth, Planetary, and Space 7 8 VS in the crust, and a fairly good Sciences, -
The Reference Mission of the NASA Mars Exploration Study Team
NASA Special Publication 6107 Human Exploration of Mars: The Reference Mission of the NASA Mars Exploration Study Team Stephen J. Hoffman, Editor David I. Kaplan, Editor Lyndon B. Johnson Space Center Houston, Texas July 1997 NASA Special Publication 6107 Human Exploration of Mars: The Reference Mission of the NASA Mars Exploration Study Team Stephen J. Hoffman, Editor Science Applications International Corporation Houston, Texas David I. Kaplan, Editor Lyndon B. Johnson Space Center Houston, Texas July 1997 This publication is available from the NASA Center for AeroSpace Information, 800 Elkridge Landing Road, Linthicum Heights, MD 21090-2934 (301) 621-0390. Foreword Mars has long beckoned to humankind interest in this fellow traveler of the solar from its travels high in the night sky. The system, adding impetus for exploration. ancients assumed this rust-red wanderer was Over the past several years studies the god of war and christened it with the have been conducted on various approaches name we still use today. to exploring Earth’s sister planet Mars. Much Early explorers armed with newly has been learned, and each study brings us invented telescopes discovered that this closer to realizing the goal of sending humans planet exhibited seasonal changes in color, to conduct science on the Red Planet and was subjected to dust storms that encircled explore its mysteries. The approach described the globe, and may have even had channels in this publication represents a culmination of that crisscrossed its surface. these efforts but should not be considered the final solution. It is our intent that this Recent explorers, using robotic document serve as a reference from which we surrogates to extend their reach, have can continuously compare and contrast other discovered that Mars is even more complex new innovative approaches to achieve our and fascinating—a planet peppered with long-term goal. -
Scientific Rationale and Requirements for a Global Seismic Network on Mars
SCIENTIFIC RATIONALE AND REQUIREMENTS FOR A GLOBAL SEISMIC NETWORK ON MARS MARS Model AR 90 EARTH 180 (NASA-CR-188806) SCIENTIFIC RATIONALE AND N92-14949 REQUIREMENTS FOR A GLOBAL SEISMIC NETWORK ON MARS (Lunar and Planetary Inst.) 48 p CSCL 03B Unclas G3/91 0040098 LPI Technical Report Number 91-02 LUNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON TX 77058-4399 LPI/TR-91-02 SCIENTIFIC RATIONALE AND REQUIREMENTS FOR A GLOBAL SEISMIC NETWORK ON MARS Sean C. Solomon, Don L. Anderson, W. Bruce Banerdt, Rhett G. Butler, Paul M. Davis, Frederick K. Duennebier, Yosio Nakamura, Emile A. Okal, and Roger J. Phillips Report of a Workshop Held at Morro Bay, California May 7-9, 1990 Lunar and Planetary Institute 3303 NASA Road 1 Houston TX 77058 LPI Technical Report Number 91-02 LPI/TR-91-02 Compiled in 1991 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4574 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Solomon S. C. et al. (1991) Scientific Rationale and Requirements far a Global Seismic Network on Mars. LPI Tech. Rpt. 91-02, Lunar and Planetary Institute, Houston. 51 pp. This report is distributed by: ORDER DEPARTMENT Lunar and Planetary Institute 3303 NASA Road 1 Houston TX 77058-4399 Mail order requestors will be invoiced for the cost of shipping and handling. -
An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger Depauw University
DePauw University Scholarly and Creative Work from DePauw University Student research Student Work 2015 An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger DePauw University Follow this and additional works at: http://scholarship.depauw.edu/studentresearch Part of the Economics Commons, and the The unS and the Solar System Commons Recommended Citation Knappenberger, Clayton, "An Economic Analysis of Mars Exploration and Colonization" (2015). Student research. Paper 28. This Thesis is brought to you for free and open access by the Student Work at Scholarly and Creative Work from DePauw University. It has been accepted for inclusion in Student research by an authorized administrator of Scholarly and Creative Work from DePauw University. For more information, please contact [email protected]. An Economic Analysis of Mars Exploration and Colonization Clayton Knappenberger 2015 Sponsored by: Dr. Villinski Committee: Dr. Barreto and Dr. Brown Contents I. Why colonize Mars? ............................................................................................................................ 2 II. Can We Colonize Mars? .................................................................................................................... 11 III. What would it look like? ............................................................................................................... 16 A. National Program ......................................................................................................................... -
Educator's Guide
EDUCATOR’S GUIDE ABOUT THE FILM Dear Educator, “ROVING MARS”is an exciting adventure that This movie details the development of Spirit and follows the journey of NASA’s Mars Exploration Opportunity from their assembly through their Rovers through the eyes of scientists and engineers fantastic discoveries, discoveries that have set the at the Jet Propulsion Laboratory and Steve Squyres, pace for a whole new era of Mars exploration: from the lead science investigator from Cornell University. the search for habitats to the search for past or present Their collective dream of Mars exploration came life… and maybe even to human exploration one day. true when two rovers landed on Mars and began Having lasted many times longer than their original their scientific quest to understand whether Mars plan of 90 Martian days (sols), Spirit and Opportunity ever could have been a habitat for life. have confirmed that water persisted on Mars, and Since the 1960s, when humans began sending the that a Martian habitat for life is a possibility. While first tentative interplanetary probes out into the solar they continue their studies, what lies ahead are system, two-thirds of all missions to Mars have NASA missions that not only “follow the water” on failed. The technical challenges are tremendous: Mars, but also “follow the carbon,” a building block building robots that can withstand the tremendous of life. In the next decade, precision landers and shaking of launch; six months in the deep cold of rovers may even search for evidence of life itself, space; a hurtling descent through the atmosphere either signs of past microbial life in the rock record (going from 10,000 miles per hour to 0 in only six or signs of past or present life where reserves of minutes!); bouncing as high as a three-story building water ice lie beneath the Martian surface today. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Mars Exploration - a Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani
Chapter Introductory Chapter: Mars Exploration - A Story Fifty Years Long Giuseppe Pezzella and Antonio Viviani 1. Introduction Mars has been a goal of exploration programs of the most important space agencies all over the world for decades. It is, in fact, the most investigated celestial body of the Solar System. Mars robotic exploration began in the 1960s of the twentieth century by means of several space probes sent by the United States (US) and the Soviet Union (USSR). In the recent past, also European, Japanese, and Indian spacecrafts reached Mars; while other countries, such as China and the United Arab Emirates, aim to send spacecraft toward the red planet in the next future. 1.1 Exploration aims The high number of mission explorations to Mars clearly points out the impor- tance of Mars within the Solar System. Thus, the question is: “Why this great interest in Mars exploration?” The interest in Mars is due to several practical, scientific, and strategic reasons. In the practical sense, Mars is the most accessible planet in the Solar System [1]. It is the second closest planet to Earth, besides Venus, averaging about 360 million kilometers apart between the furthest and closest points in its orbit. Earth and Mars feature great similarities. For instance, both planets rotate on an axis with quite the same rotation velocity and tilt angle. The length of a day on Earth is 24 h, while slightly longer on Mars at 24 h and 37 min. The tilt of Earth axis is 23.5 deg, and Mars tilts slightly more at 25.2 deg [2]. -
Mars Field Geology, Biology, and Paleontology Workshop, Summary
MARS FIELD GEOLOGY, BIOLOGY, AND PALEONTOLOGY WORKSHOP: SUMMARY AND RECOMMENDATIONS November 18–19, 1998 Space Center Houston, Houston, Texas LPI Contribution No. 968 MARS FIELD GEOLOGY, BIOLOGY, AND PALEONTOLOGY WORKSHOP: SUMMARY AND RECOMMENDATIONS November 18–19, 1998 Space Center Houston Edited by Nancy Ann Budden Lunar and Planetary Institute Sponsored by Lunar and Planetary Institute National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Contribution No. 968 Compiled in 1999 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautcis and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This volume may be cited as Budden N. A., ed. (1999) Mars Field Geology, Biology, and Paleontology Workshop: Summary and Recommendations. LPI Contribution No. 968, Lunar and Planetary Institute, Houston. 80 pp. This volume is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Phone: 281-486-2172 Fax: 281-486-2186 E-mail: [email protected] Mail order requestors will be invoiced for the cost of shipping and handling. _________________ Cover: Mars test suit subject and field geologist Dean Eppler overlooking Meteor Crater, Arizona, in Mark III Mars EVA suit. PREFACE In November 1998 the Lunar and Planetary Institute, under the sponsorship of the NASA/HEDS (Human Exploration and Development of Space) Enterprise, held a workshop to explore the objectives, desired capabilities, and operational requirements for the first human exploration of Mars. -
Seasonal and Interannual Variability of Solar Radiation at Spirit, Opportunity and Curiosity Landing Sites
Seasonal and interannual variability of solar radiation at Spirit, Opportunity and Curiosity landing sites Álvaro VICENTE-RETORTILLO1, Mark T. LEMMON2, Germán M. MARTÍNEZ3, Francisco VALERO4, Luis VÁZQUEZ5, Mª Luisa MARTÍN6 1Departamento de Física de la Tierra, Astronomía y Astrofísica II, Universidad Complutense de Madrid, Madrid, Spain, [email protected]. 2Department of Atmospheric Sciences, Texas A&M University, College Station, TX, USA, [email protected]. 3Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, USA, [email protected]. 4Departamento de Física de la Tierra, Astronomía y Astrofísica II, Universidad Complutense de Madrid, Madrid, Spain, [email protected]. 5Departamento de Matemática Aplicada, Universidad Complutense de Madrid, Madrid, Spain, [email protected]. 6Departamento de Matemática Aplicada, Universidad de Valladolid, Segovia, Spain, [email protected]. Received: 14/04/2016 Accepted: 22/09/2016 Abstract In this article we characterize the radiative environment at the landing sites of NASA's Mars Exploration Rover (MER) and Mars Science Laboratory (MSL) missions. We use opacity values obtained at the surface from direct imaging of the Sun and our radiative transfer model COMIMART to analyze the seasonal and interannual variability of the daily irradiation at the MER and MSL landing sites. In addition, we analyze the behavior of the direct and diffuse components of the solar radiation at these landing sites. Key words: Solar radiation; Mars Exploration Rovers; Mars Science Laboratory; opacity, dust; radiative transfer model; Mars exploration. Variabilidad estacional e interanual de la radiación solar en las coordenadas de aterrizaje de Spirit, Opportunity y Curiosity Resumen El presente artículo está dedicado a la caracterización del entorno radiativo en los lugares de aterrizaje de las misiones de la NASA de Mars Exploration Rover (MER) y de Mars Science Laboratory (MSL). -
Magnitude Scales for Marsquakes
Bulletin of the Seismological Society of America, Vol. XX, No. XX, pp. –, – 2018, doi: 10.1785/0120180037 Ⓔ Magnitude Scales for Marsquakes by Maren Böse,* Domenico Giardini, Simon Stähler, Savas Ceylan, John Francis Clinton, Martin van Driel, Amir Khan, Fabian Euchner, Philippe Lognonné, and William Bruce Banerdt Abstract In anticipation of the upcoming 2018 InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) Discovery mission to Mars, we calibrate magnitude scales for marsquakes that incorporate state-of-the-art knowledge on Mars interior structure and the expected ambient and instrumental noise. We re- gress magnitude determinations of 2600 randomly distributed marsquakes, simulated with a spectral element method for 13 published 1D structural models of Mars’ interior. The continuous seismic data from InSight will be returned at 2 samples per second. To account for this limited bandwidth as well as for the expected noise conditions on Mars, we define and calibrate six magnitude scales: (1) local Mars mag- MMa nitude L at a period of 3 s for marsquakes at distances of up to 10°; (2) P-wave mMa mMa magnitude b ; (3) S-wave magnitude bS each defined at a period of 3 s and cali- MMa brated for distances from 5° to 100°; (4) surface-wave magnitude s defined at a MMa MMa period of 20 s, as well as (5) moment magnitudes FB ; and (6) F computed from the low-frequency (10–100 s) plateau of the displacement spectrum for either body waves or body and surface waves, respectively; we calibrate scales (4)–(6) for dis- tances from 5° to 180°.