MARS SURVEYOR PROGRAM 2001 MISSION OVERVIEW. R. Stephen
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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. -
MARS an Overview of the 1985–2006 Mars Orbiter Camera Science
MARS MARS INFORMATICS The International Journal of Mars Science and Exploration Open Access Journals Science An overview of the 1985–2006 Mars Orbiter Camera science investigation Michael C. Malin1, Kenneth S. Edgett1, Bruce A. Cantor1, Michael A. Caplinger1, G. Edward Danielson2, Elsa H. Jensen1, Michael A. Ravine1, Jennifer L. Sandoval1, and Kimberley D. Supulver1 1Malin Space Science Systems, P.O. Box 910148, San Diego, CA, 92191-0148, USA; 2Deceased, 10 December 2005 Citation: Mars 5, 1-60, 2010; doi:10.1555/mars.2010.0001 History: Submitted: August 5, 2009; Reviewed: October 18, 2009; Accepted: November 15, 2009; Published: January 6, 2010 Editor: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University Reviewers: Jeffrey B. Plescia, Applied Physics Laboratory, Johns Hopkins University; R. Aileen Yingst, University of Wisconsin Green Bay Open Access: Copyright 2010 Malin Space Science Systems. This is an open-access paper distributed under the terms of a Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Abstract Background: NASA selected the Mars Orbiter Camera (MOC) investigation in 1986 for the Mars Observer mission. The MOC consisted of three elements which shared a common package: a narrow angle camera designed to obtain images with a spatial resolution as high as 1.4 m per pixel from orbit, and two wide angle cameras (one with a red filter, the other blue) for daily global imaging to observe meteorological events, geodesy, and provide context for the narrow angle images. Following the loss of Mars Observer in August 1993, a second MOC was built from flight spare hardware and launched aboard Mars Global Surveyor (MGS) in November 1996. -
Gulick, V CV2008.PDF
Curriculum Vitae: Dr. Virginia C. Gulick Nr\SA Amcs RcsearchCenter, lVfail Stop 239-20,Moffetl Field, Califoniia94035 (650) 604-0781 (office), Vireinia.C.GuUckr7lnase-gav IIDUCATION PhD (Geosciences);University of Arizona Ph.D. Thesis: Magnmtic Intrusiorts ancl l{ydrotlrcrmal Systents:Implicatiotts for the Fornmtion of Small Msrtian Valleys MS. (Geosciencr:s),Minor in Hydrology,The University of Arizona,Tucson Master Thesis: Origin ad Ev'olutionoJ'I'alle1's on the Martian Volcanoes:T'he Hatvaiittn.4nalog. B.A. (Geoscicnces),Rutgers University (Rutgers College) New Brunswick, New Jersey Senior Thesis:TIte Coral SeaSedinettt Study. I'[t.ft]SENTPOStrTION 1996-prres.:ResearchScientist (SETI InstitutePrincipal Investigator)& Adjunct Professor,Astronomy Dept.,NM StateUniv. u Mars ScienceLab 2009landing site selcction steering group nrembcr. r MRO'05 IIiRISE instrumentsciencc ternr nrcnibcr(200)-2009): Lead on flrn,ial & hydrothernral processes, E/PO & r'r,eb technologies. I-IiRl:iE E/PO website (http://nrarsox,eb.nas.uasa. gov/I{iRISE) presentation Planctary l)ata in E,ducational ' Invited to AGU's Scssion Using Settings. Presentationtitle: "MRO's High Re.solutionImaging ScienceExperirncnt ([iiRISE): EdLrcation And PubiicOutr each Plans",. r Invitedpanelist fot NASA's Leamingfiom the Frontier:Getting Planetary l)ata into the Herndsof EducatorsWorkshop at LPi, March 14,2004. ' Co-convcuerof thc Volcano/iceInteraction on Earthand Mars Conf-.,P.eykjavik, Iceland, August 2000. " Projectscicnce lead on Marsorveb:the Mars l,anding Site Studies& Global Visualizationweb cnvironmentr:ffort (hItpJ4UDSIylb.nas.liUagq1llandinqsites).1998-present. o ScienceCoI for the Clickworkersl'roject; NASA's Experimeutin distributeddata analysis by the p ubl i c w eb si tc (liltd&lekfi g*9t$.3l9.qag4.gev ) 20 0 0-p resent. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
Solarhub Maxar’S Lunar Vertical Solar Array Technology
SolarHub Maxar’s Lunar Vertical Solar Array Technology Presented to the Lunar Surface Innovation Consortium (LSIC) 2021-05-27 Approved for External Release MAXAR AND LUNAR EXPLORATION Solar Power Use or disclosure of the data contained on this sheet © 2021 Maxar Technologies 2 is subject to the restrictions on the cover page A MISSION PARTNER WITH PROVEN HERITAGE With more than 60 years of experience, Maxar is a trusted partner for government and commercial missions. Our renowned Space Infrastructure capabilities date back to the Apollo Moon landing and continue to serve the most demanding missions: ▪ Communications and Earth observation ▪ Space exploration ▪ Solar electric propulsion ▪ On-orbit servicing and assembly 285+ 2,750 80+ 2.4+ Maxar-built spacecraft Combined Communication Billion people rely on launched years on orbit satellites on orbit broadcasting services powered by Maxar-built satellites Use or disclosure of the data contained on this sheet © 2021 Maxar Technologies is subject to the restrictions on the cover page 3 MAXAR IS A GLOBALLY TRUSTED LEADER DELIVERING SPACE INFRASTRUCTURE AND EARTH INTELLIGENCE SPACE INFRASTRUCTURE EARTH INTELLIGENCE Use or disclosure of the data contained on this sheet © 2021 Maxar Technologies 4 is subject to the restrictions on the cover page Psyche spacecraft chassis, power & MAXAR SPACE INFRASTRUCTURE propulsion ▪ 60+ years building high reliability spacecraft ▪ Launched 285+ LEO & GEO satellites ▪ Leader in Solar Electric Propulsion (SEP) ▪ High heritage in: − power management and distribution -
The Mars Surveyor Program - Planned Orbiter and Lander for 2001
Lunar and Planetary Science XXXI 1776.pdf THE MARS SURVEYOR PROGRAM - PLANNED ORBITER AND LANDER FOR 2001. R. S. Saunders, Jet Propulsion Laboratory, 180-701, 4800 Oak Grove Drive, Pasadena, CA 91109, [email protected]. Introduction: Following the loss of the Mars Cli- An additional experiment, the Martian Radiation mate Orbiter and the Mars Polar Lander, the Mars Environment Experiment (MARIE) is an energetic Surveyor Program is undergoing a replanning effort. particle spectrometer designed to measure the near There is currently no anticipated change to the 2001 space radiation environment as related to the radiation orbiter science payload, which is scheduled for launch hazard to human explorers. This is one of the Human on March 30, 2001. If launched on schedule, the or- Exploration and Development of Space Enterprise biter will arrive at Mars on Oct. 20, 2001. The 2001 (HEDS) experiments that was selected for the 2001 orbiter carries the Gamma Ray Spectrometer (GRS) mission to acquire data needed before planning human (based on science objectives lost with Mars Observer) missions to Mars. MARIE will determine the radia- and the Thermal Emission Imaging System tion energy spectrum, separate the contribution from (THEMIS). The Mars Surveyor 2001 Lander is sched- various particles, and measure the accumulated ab- uled to launch on April 10, 2001 and will land on sorbed dose and dose rate that would occur in human Mars on January 22, 2002, about three months after tissue. the orbiter arrives and about two weeks after the or- Lander Site Selection: During the past year, the biter achieves its mapping orbit following a 76 day planetary science community was engaged in selecting aerobraking sequence. -
Mars Exploration Entry, Descent and Landing Challenges1,2
Mars Exploration Entry, Descent and Landing Challenges1,2 Robert D. Braun Robert M. Manning Georgia Institute of Technology Jet Propulsion Laboratory Atlanta, GA 30332-0150 California Institute of Technology (404) 385-6171 Pasadena, CA 91109 [email protected] (818) 393-7815 [email protected] Abstract—The United States has successfully landed five interesting locations within close proximity (10’s of m) of robotic systems on the surface of Mars. These systems all pre-positioned robotic assets. These plans require a had landed mass below 0.6 metric tons (t), had landed simultaneous two order of magnitude increase in landed footprints on the order of hundreds of km and landed at sites mass capability, four order of magnitude increase in landed below -1 km MOLA elevation due the need to perform accuracy, and an entry, descent and landing operations entry, descent and landing operations in an environment sequence that may need to be completed in a lower density with sufficient atmospheric density. Current plans for (higher surface elevation) environment. This is a tall order human exploration of Mars call for the landing of 40-80 t that will require the space qualification of new EDL surface elements at scientifically interesting locations within approaches and technologies. close proximity (10’s of m) of pre-positioned robotic assets. This paper summarizes past successful entry, descent and Today, robotic exploration systems engineers are struggling landing systems and approaches being developed by the with the challenges of increasing landed mass capability to 1 robotic Mars exploration program to increased landed t while improving landed accuracy to 10’s of km and performance (mass, accuracy and surface elevation). -
Proposal Information Package
NASA RESEARCH ANNOUNCEMENT PROPOSAL INFORMATION PACKAGE Mars Exploration Program 2001 Mars Odyssey Orbiter 23 July 2001 Contributors Raymond Arvidson1 Jeffrey J. Plaut5 Gautam Badhwar2 Susan Slavney1 William Boynton3 David A. Spencer5 Philip Christensen4 Compiled by Thomas W. Thompson5 Jeffrey J. Plaut5 Catherine M. Weitz6 1Washington University, 2Johnson Space Center, 3Lunar and Planetary Laboratory (University of Arizona), 4Arizona State University, 5Jet Propulsion Laboratory, California Institute of Technology 6NASA Headquarters. Table of Contents 1.0 Overview..............................................................................................................................................................1-1 1.1 Document Overview.............................................................................................................................1-1 1.2 Mars Exploration Program...................................................................................................................1-1 1.3 Mars 2001 Objectives...........................................................................................................................1-2 1.4 Mars 2001 Operations Management....................................................................................................1-2 1.5 Mars 2001 Orbiter Measurement Synergies through Coordinated Operations Planning ..................1-2 1.6 Mars 2001 Project Science Group (PSG) Members............................................................................1-3 2.0 Mars -
Locations of Anthropogenic Sites on the Moon R
Locations of Anthropogenic Sites on the Moon R. V. Wagner1, M. S. Robinson1, E. J. Speyerer1, and J. B. Plescia2 1Lunar Reconnaissance Orbiter Camera, School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-3603; [email protected] 2The Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723 Abstract #2259 Introduction Methods and Accuracy Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera To get the location of each object, we recorded its line and sample in (NAC) images, with resolutions from 0.25-1.5 m/pixel, allow the each image it appears in, and then used USGS ISIS routines to extract identifcation of historical and present-day landers and spacecraft impact latitude and longitude for each point. The true position is calculated to be sites. Repeat observations, along with recent improvements to the the average of the positions from individual images, excluding any extreme spacecraft position model [1] and the camera pointing model [2], allow the outliers. This process used Spacecraft Position Kernels improved by LOLA precise determination of coordinates for those sites. Accurate knowledge of cross-over analysis and the GRAIL gravity model, with an uncertainty of the coordinates of spacecraft and spacecraft impact craters is critical for ±10 meters [1], and a temperature-corrected camera pointing model [2]. placing scientifc and engineering observations into their proper geologic At sites with a retrorefector in the same image as other objects (Apollo and geophysical context as well as completing the historic record of past 11, 14, and 15; Luna 17), we can improve the accuracy signifcantly. Since trips to the Moon. -
The Mars Global Surveyor Mars Orbiter Camera: Interplanetary Cruise Through Primary Mission
p. 1 The Mars Global Surveyor Mars Orbiter Camera: Interplanetary Cruise through Primary Mission Michael C. Malin and Kenneth S. Edgett Malin Space Science Systems P.O. Box 910148 San Diego CA 92130-0148 (note to JGR: please do not publish e-mail addresses) ABSTRACT More than three years of high resolution (1.5 to 20 m/pixel) photographic observations of the surface of Mars have dramatically changed our view of that planet. Among the most important observations and interpretations derived therefrom are that much of Mars, at least to depths of several kilometers, is layered; that substantial portions of the planet have experienced burial and subsequent exhumation; that layered and massive units, many kilometers thick, appear to reflect an ancient period of large- scale erosion and deposition within what are now the ancient heavily cratered regions of Mars; and that processes previously unsuspected, including gully-forming fluid action and burial and exhumation of large tracts of land, have operated within near- contemporary times. These and many other attributes of the planet argue for a complex geology and complicated history. INTRODUCTION Successive improvements in image quality or resolution are often accompanied by new and important insights into planetary geology that would not otherwise be attained. From the variety of landforms and processes observed from previous missions to the planet Mars, it has long been anticipated that understanding of Mars would greatly benefit from increases in image spatial resolution. p. 2 The Mars Observer Camera (MOC) was initially selected for flight aboard the Mars Observer (MO) spacecraft [Malin et al., 1991, 1992]. -
Exobiology in the Solar System & the Search for Life on Mars
SP-1231 SP-1231 October 1999 Exobiology in the Solar System & The Search for Life on Mars for The Search Exobiology in the Solar System & Exobiology in the Solar System & The Search for Life on Mars Report from the ESA Exobiology Team Study 1997-1998 Contact: ESA Publications Division c/o ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands Tel. (31) 71 565 3400 - Fax (31) 71 565 5433 SP-1231 October 1999 EXOBIOLOGY IN THE SOLAR SYSTEM AND THE SEARCH FOR LIFE ON MARS Report from the ESA Exobiology Team Study 1997-1998 Cover Fossil coccoid bacteria, 1 µm in diameter, found in sediment 3.3-3.5 Gyr old from the Early Archean of South Africa. See pages 160-161. Background: a portion of the meandering canyons of the Nanedi Valles system viewed by Mars Global Surveyor. The valley is about 2.5 km wide; the scene covers 9.8 km by 27.9 km centred on 5.1°N/48.26°W. The valley floor at top right exhibits a 200 m-wide channel covered by dunes and debris. This channel suggests that the valley might have been carved by water flowing through the system over a long period, in a manner similar to rivers on Earth. (Malin Space Science Systems/NASA) SP-1231 ‘Exobiology in the Solar System and The Search for Life on Mars’, ISBN 92-9092-520-5 Scientific Coordinators: André Brack, Brian Fitton and François Raulin Edited by: Andrew Wilson ESA Publications Division Published by: ESA Publications Division ESTEC, Noordwijk, The Netherlands Price: 70 Dutch Guilders/ EUR32 Copyright: © 1999 European Space Agency Contents Foreword 7 I An Exobiological View of the -
Risk Assessment Applications to Science and Explorationsmissions
RISK ASSESSMENT APPLICATIONS TO SCIENCE AND EXPLORATION MISSIONS Dr. Todd Paulos [email protected] Risk Analysis of Aerospace Missions II: Mission Success Starts with Safety Workshop Key Bridge Marriott Arlington, Virginia October 29, 2002 Introduction z Brief PRA Review z Exploration Missions z Mars ’03 z Mars ’07 z Mars ’09 z MSR (Mars ’13? Or Mars ‘not in my lifetime) z Science Missions z CloudSAT z GRACE z Herschel Planck z Summary SRA, October 29, 2002 T. Paulos 2 Brief PRA Review Inputs to Decision Making Process Master Logic Diagram (Hierarchical Logic) Event Sequence Diagram (Logic) IE End State: ES1 A B End State: OK EndEnd State: State: ES2 ES2 End State: ES2 C D E End State: ES1 End State: ES2 Event Tree (Inductive Logic) Fault Tree (Logic) One to Many Mapping of an ET-defined Scenario End Not A IE A B C D E NEW STRUCTURE State LOGIC MODELING Logic Gate 1: OK Basic Event Internal initiating events One of these events External initiating events 2: ES1 Hardware components AND 3: ES2 Human error 4: ES2 Software error one or more Common cause of these 5: ES2 elementary Environmental conditions events 6: ES2 Other Link to another fault tree Probabilistic Treatment of Basic Events Model Integration and Quantification of Risk Scenarios Risk Results and Insights 30 50 60 25 50 40 End State: ES2 Integration and quantification of 20 40 30 100 logic structures (ETs and FTs) 30 15 Displaying the results in tabular and graphical forms 10 20 80 and propagation of epistemic 20 uncertainties to obtain Ranking of risk scenarios 10