Geologic Constraints on Early Mars Climate
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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 -
Wind-Eroded Stratigraphy on the Floor of a Noachian Impact Crater, Noachis Terra, Mars
Third Conference on Early Mars (2012) 7066.pdf WIND-ERODED STRATIGRAPHY ON THE FLOOR OF A NOACHIAN IMPACT CRATER, NOACHIS TERRA, MARS. R. P. Irwin III1,2, J. J. Wray3, T. A. Maxwell1, S. C. Mest2,4, and S. T. Hansen3, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, MRC 315, 6th St. at Independence Ave. SW, Washington DC 20013, [email protected], [email protected]. 2Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson AZ 85719, [email protected]. 3School of Earth and Atmospheric Sciences, Georgia Institute of Technology, 311 Ferst Drive, Atlanta GA 30332-0340, [email protected], [email protected]. 4Planetary Geodynamics Laboratory, Code 698, NASA Goddard Space Flight Center, Greenbelt MD 20771. Introduction: Detailed stratigraphic and spectral cular 12-km depression (a possible highly degraded studies of outcrops exposed in craters and other basins crater) on the southern side. The former received in- have significantly advanced the understanding of early ternal drainage from the north and east, whereas part Mars. Most studies have focused on high-relief sec- of the southern wall drained to the latter (Fig. 2). tions exposed by aeolian deflation, such as those in Gale crater, Arabia Terra, and Valles Marineris [1–3]. Many flat-floored Noachian degraded craters also have wind-eroded strata, suggesting that they lack a cap rock of Gusev-type basalts [4,5]. This study focuses on the youngest materials exposed on the wind-eroded floor of an unnamed Noachian degraded crater in Noachis Terra, Mars. The crater is centered at 20.2ºS, 42.6ºE and is 52 km in diameter. -
Chapter 4 Ild Observations in Valles Marineris and Chaotic Terrains
46 CHAPTER 4 ILD OBSERVATIONS IN VALLES MARINERIS AND CHAOTIC TERRAINS ILDs have been found and analysed in locations in Valles Marineris and in the chaotic terrains that lie east of Valles Marineris, from 18°S/309°E to 5°N/343°E. Ganges and Capri/Eos Chasma are related to chaotic terrain and outflow channels as well (Sect. 2.4). Even within the Valles Marineris, ILDs are enclosed by chaotic terrain. ILDs are often found in the form of erosional remnants as mesas or buttes (Sect. 2.4.3, 2.5). Exposures in the Ganges and Capri Chasmata as well as in Aurorae, Arsinoes, Aureum, Aram, and Iani Chaos (Fig. 28) were analysed in this thesis. Figure 28: MOLA map of the research area. The research area is located in the eastern Valles Marineris and the Margaritifer Terra chaotic terrains. ILDs that are found and analysed are marked black and are situated between 18°S/309°E to 5°N/343°E. 4.1 Chaotic Terrains 47 4.1 CHAOTIC TERRAINS 4.1.1 Aram Chaos Aram Chaos (3°N/338.8°E) is a 280 km-wide circular structure that is located between the Ares Vallis outflow channel to the east and Aureum Chaos, and Iani Chaos (Fig. 28). The ILD material measures 120 by 140 km and is located near the crater centre (Fig. 29). Elevation ranges from -3700 m to -2900 m (Fig. 31C). Figure 29: Aram Chaos impact crater (centred 3°N/338.8°E) exhibiting ILD material superimposed on heavily disrupted chaotic terrain. To the east, there is a gorge that empties into Ares Vallis (Fig. -
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. -
Evidence for Thermal-Stress-Induced Rockfalls on Mars Impact Crater Slopes
Icarus 342 (2020) 113503 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Evidence for thermal-stress-induced rockfalls on Mars impact crater slopes P.-A. Tesson a,b,*, S.J. Conway b, N. Mangold b, J. Ciazela a, S.R. Lewis c, D. M�ege a a Space Research Centre, Polish Academy of Science, Wrocław, Poland b Laboratoire de Plan�etologie et G�eodynamique UMR 6112, CNRS, Nantes, France c School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK ARTICLE INFO ABSTRACT Keywords: Here we study rocks falling from exposed outcrops of bedrock, which have left tracks on the slope over which Mars, surface they have bounced and/or rolled, in fresh impact craters (1–10 km in diameter) on Mars. The presence of these Thermal stress tracks shows that these rocks have fallen relatively recently because aeolian processes are known to infill Ices topographic lows over time. Mapping of rockfall tracks indicate trends in frequency with orientation, which in Solar radiation � � turn depend on the latitudinal position of the crater. Craters in the equatorial belt (between 15 N and 15 S) Weathering exhibit higher frequencies of rockfall on their north-south oriented slopes compared to their east-west ones. � Craters >15 N/S have notably higher frequencies on their equator-facing slopes as opposed to the other ori entations. We computed solar radiation on the surface of crater slopes to compare insolation patterns with the spatial distribution of rockfalls, and found statistically significant correlations between maximum diurnal inso lation and rockfall frequency. -
Mars, the Nearest Habitable World – a Comprehensive Program for Future Mars Exploration
Mars, the Nearest Habitable World – A Comprehensive Program for Future Mars Exploration Report by the NASA Mars Architecture Strategy Working Group (MASWG) November 2020 Front Cover: Artist Concepts Top (Artist concepts, left to right): Early Mars1; Molecules in Space2; Astronaut and Rover on Mars1; Exo-Planet System1. Bottom: Pillinger Point, Endeavour Crater, as imaged by the Opportunity rover1. Credits: 1NASA; 2Discovery Magazine Citation: Mars Architecture Strategy Working Group (MASWG), Jakosky, B. M., et al. (2020). Mars, the Nearest Habitable World—A Comprehensive Program for Future Mars Exploration. MASWG Members • Bruce Jakosky, University of Colorado (chair) • Richard Zurek, Mars Program Office, JPL (co-chair) • Shane Byrne, University of Arizona • Wendy Calvin, University of Nevada, Reno • Shannon Curry, University of California, Berkeley • Bethany Ehlmann, California Institute of Technology • Jennifer Eigenbrode, NASA/Goddard Space Flight Center • Tori Hoehler, NASA/Ames Research Center • Briony Horgan, Purdue University • Scott Hubbard, Stanford University • Tom McCollom, University of Colorado • John Mustard, Brown University • Nathaniel Putzig, Planetary Science Institute • Michelle Rucker, NASA/JSC • Michael Wolff, Space Science Institute • Robin Wordsworth, Harvard University Ex Officio • Michael Meyer, NASA Headquarters ii Mars, the Nearest Habitable World October 2020 MASWG Table of Contents Mars, the Nearest Habitable World – A Comprehensive Program for Future Mars Exploration Table of Contents EXECUTIVE SUMMARY .......................................................................................................................... -
Mid-Latitude Ice on Mars: a Science Target for Planetary Climate Histories and an Exploration Target for in Situ Resources
Mid-Latitude Ice on Mars: A Science Target for Planetary Climate Histories and an Exploration Target for In Situ Resources A White Paper submitted to the Planetary Sciences Decadal Survey 2023–2032 Primary Contact: Ali M. Bramson, Purdue University ([email protected]) Authors: Ali M. Bramson1,2 John (Jack) W. Holt2 Eric I. Petersen2,12 Chimira Andres3 Suniti Karunatillake8 Nathaniel E. Putzig6 Jonathan Bapst4 Aditya Khuller9 Hanna G. Sizemore6 Patricio Becerra5 Michael T. Mellon10 Isaac B. Smith6,13 Samuel W. Courville6 Gareth A. Morgan6 David E. Stillman14 Colin M. Dundas7 Rachel W. Obbard11 Paul Wooster15 Shannon M. Hibbard3 Matthew R. Perry6 1Purdue University, 2University of Arizona, 3University of Western Ontario CA, 4Jet Propulsion Laboratory, California Institute of Technology, 5University of Bern CH, 6Planetary Science Institute, 7U.S. Geological Survey, 8Louisiana State University, 9Arizona State University, 10Cornell University, 11SETI Institute, 12University of Alaska Fairbanks, 13York University, 14Southwest Research Institute, 15SpaceX Signatories: Ken Herkenhoff, U.S. Geological Survey Alfred McEwen, U. of Arizona David M. Hollibaugh Baker, NASA GSFC Wendy Calvin, U. of Nevada Reno Stefano Nerozzi, U. of Arizona Nicolas Thomas, U. of Bern, CH Serina Diniega, NASA JPL Paul Hayne, U. of Colorado Boulder Jeffrey Plaut, NASA JPL/Caltech Kim Seelos, JHU/APL Charity Phillips-Lander, SwRI Shane Byrne, U. of Arizona Cynthia Dinwiddie, SwRI Devanshu Jha, MVJ College of Eng., IN Aymeric Spiga, LMD/Sorbonne Université, FR Michael S. Veto, Ball Aerospace Andreas Johnsson, U. of Gothenburg, SE Matthew Chojnacki, PSI Michael Mischna, NASA JPL/Caltech Jacob Widmer, Representing Self Adrian J. Brown, Plancius Research, LLC Carol Stoker, NASA Ames Noora Alsaeed, CU Boulder, LASP Alberto G. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Workshop on the Martiannorthern Plains: Sedimentological,Periglacial, and Paleoclimaticevolution
NASA-CR-194831 19940015909 WORKSHOP ON THE MARTIANNORTHERN PLAINS: SEDIMENTOLOGICAL,PERIGLACIAL, AND PALEOCLIMATICEVOLUTION MSATT ..V",,2' :o_ MarsSurfaceandAtmosphereThroughTime Lunar and PlanetaryInstitute 3600 Bay AreaBoulevard Houston TX 77058-1113 ' _ LPI/TR--93-04Technical, Part 1 Report Number 93-04, Part 1 L • DISPLAY06/6/2 94N20382"£ ISSUE5 PAGE2088 CATEGORY91 RPT£:NASA-CR-194831NAS 1.26:194831LPI-TR-93-O4-PT-ICNT£:NASW-4574 93/00/00 29 PAGES UNCLASSIFIEDDOCUMENT UTTL:Workshopon the MartianNorthernPlains:Sedimentological,Periglacial, and PaleoclimaticEvolution TLSP:AbstractsOnly AUTH:A/KARGEL,JEFFREYS.; B/MOORE,JEFFREY; C/PARKER,TIMOTHY PAA: A/(GeologicalSurvey,Flagstaff,AZ.); B/(NationalAeronauticsand Space Administration.GoddardSpaceFlightCenter,Greenbelt,MD.); C/(Jet PropulsionLab.,CaliforniaInst.of Tech.,Pasadena.) PAT:A/ed.; B/ed.; C/ed. CORP:Lunarand PlanetaryInst.,Houston,TX. SAP: Avail:CASIHC A03/MFAOI CIO: UNITEDSTATES Workshopheld in Fairbanks,AK, 12-14Aug.1993;sponsored by MSATTStudyGroupandAlaskaUniv. MAJS:/*GLACIERS/_MARSSURFACE/*PLAINS/*PLANETARYGEOLOGY/*SEDIMENTS MINS:/ HYDROLOGICALCYCLE/ICE/MARS CRATERS/MORPHOLOGY/STRATIGRAPHY ANN: Papersthathavebeen acceptedforpresentationat the Workshopon the MartianNorthernPlains:Sedimentological,Periglacial,and Paleoclimatic Evolution,on 12-14Aug. 1993in Fairbanks,Alaskaare included.Topics coveredinclude:hydrologicalconsequencesof pondedwateron Mars; morpho!ogical and morphometric studies of impact cratersin the Northern Plainsof Mars; a wet-geology and cold-climateMarsmodel:punctuation -
Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J. -
The Alkaline Volcanic Rocks of Craters of the Moon National Monument, Idaho and the Columbia Hills of Gusev Crater, Mars Details
The alkaline volcanic rocks of Craters of the Moon National Monument, Idaho and the Columbia Hills of Gusev Crater, Mars Details Meeting 2016 Fall Meeting Section Planetary Sciences Session Terrestrial Analogs for Planetary Processes: Oceans, Volcanoes, Impacts, and Dunes I Identifier P31E-01 Authors Haberle, C W*, Mars Space Flight Facility, Arizona State University, Tempe, AZ, United States Hughes, S S, Idaho State University, Idaho Falls, ID, United States Kobs-Nawotniak, S E, Department of Geosciences, Idaho State University, Idaho Falls, ID, United States Christensen, P R, Arizona State University, Tempe, AZ, United States Index Sediment transport [4558] Terms Atmospheres [5405] Titan [6281] Venus [6295] Abstract Idaho's Eastern Snake River Plain (ESRP) is host to extensive expressions of basaltic volcanism dominated by non evolved olivine tholeiites (NEOT) with localized occurrences of evolved lavas. Craters of the Moon National Monument (COTM) is a polygenetic lava field comprised of more than 60 lava flows emplaced during 8 eruptive periods spanning the last 15 kyrs. The most recent eruptive period (period A; 2500-2000 yr B.P.) produced flows with total alkali vs. silica classifications spanning basalt to trachyte. Coeval with the emplacement of the COTM period A volcanic pile was the emplacement of the Wapi and Kings Bowl NEOT 70 km SSE of COTM along the Great Rift. Previous investigations have determined a genetic link between these two compositionally distinct volcanic centers where COTM compositions can be generated from NEOT melts through complex ascent paths and variable degrees of fractionation and assimilation of lower-middle crustal materials. The Mars Exploration Rover, Spirit, conducted a robotic investigation of Gusev crater from 2004-2010. -
Bio-Preservation Potential of Sediment in Eberswalde Crater, Mars
Western Washington University Western CEDAR WWU Graduate School Collection WWU Graduate and Undergraduate Scholarship Fall 2020 Bio-preservation Potential of Sediment in Eberswalde crater, Mars Cory Hughes Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/wwuet Part of the Geology Commons Recommended Citation Hughes, Cory, "Bio-preservation Potential of Sediment in Eberswalde crater, Mars" (2020). WWU Graduate School Collection. 992. https://cedar.wwu.edu/wwuet/992 This Masters Thesis is brought to you for free and open access by the WWU Graduate and Undergraduate Scholarship at Western CEDAR. It has been accepted for inclusion in WWU Graduate School Collection by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. Bio-preservation Potential of Sediment in Eberswalde crater, Mars By Cory M. Hughes Accepted in Partial Completion of the Requirements for the Degree Master of Science ADVISORY COMMITTEE Dr. Melissa Rice, Chair Dr. Charles Barnhart Dr. Brady Foreman Dr. Allison Pfeiffer GRADUATE SCHOOL David L. Patrick, Dean Master’s Thesis In presenting this thesis in partial fulfillment of the requirements for a master’s degree at Western Washington University, I grant to Western Washington University the non-exclusive royalty-free right to archive, reproduce, distribute, and display the thesis in any and all forms, including electronic format, via any digital library mechanisms maintained by WWU. I represent and warrant this is my original work, and does not infringe or violate any rights of others. I warrant that I have obtained written permissions from the owner of any third party copyrighted material included in these files.