Potential Exploration Zones for Human Missions to the Surface of Mars

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Potential Exploration Zones for Human Missions to the Surface of Mars 180° E 210° E 240° E 270° E 300° E 330° E 0° E 30° E 60° E 90° E 120° E 150° E 180° E 57° 57° V ASTIT AS BOREALI S 50° 50° ARCADI A A CID ALI A Protonilus ARCADIA Acheron Tempe UTOP IA PLANITIA PL ANIT I A Deuteronilus Mensae Fossae 56 TEMPE 53 PLANITIA Terra 44 11b Mensae PL ANITIA 11a 33 2 TERRA Phlegra Erberus 27 Montes CHR YSE Ismenius Dorsa 30° Valles Lacus Nili 30° PL ANI TIA Mawrth AMAZO N I S Chryse/ Marineris Hebrus 45b 9 Fossae Vallis ERRA Valles Viking 19 Mouth 25. T 10 OLYMPUS Kasei 6 12 PLANITIA Valles McLaughlin 34 ISIDIS MONS Jezero Hypanis ARABIA LUNAE Crater Cerberus 51 CraterSYRTIS MAJOR Vallis 17 TERRA PLANITIA Firsoff E L YSI UM PL ANUM Eastern Meridiani PLANITIA XANT H E MONTES 48 Crater SABAEA PLANUM Gale Valles. MERIDIANI PLPlanumANUM 0° Noctis 26 30 Crater 0° 42 Marineris Aram 57 LUCUS 20, 22 LUCUS RSIS Landing Coprates 54 PLANUM T ERRA 40 OPHIR THA 50 Chaos Huygens PLANUM Chasma . Southern Apollinaris M ARGARITIFER. PLANUM ORAE . Crater VALLES AUR Meridiani Sulci SYRIA 36 ANUM Sinus 7 PL TYRRHENA 46 43 SINAI TERRA 32 PLANUM 8 MARINERIS Meridiani PLANUMelasM HESPERIA Chasma 23 Equatorial. D AED ALI A P L ANUM Columbus THAUMASIA TERRA Gusev Vallis Hadriacus Crater SOLIS Ausonia Crater PLANUM Marineris 52 PLANUM PLANUM Palus 41 Cavus –30° 5 –30° 45a TERRA SouthernBOSPOROS NOA CHIS Hellas T ERRA PLANUM Newton Nectaris 28 Noachis 35 Rim MesopotamiaHELL AS 37 Crater 15 Fossae Hale Terra 38 Eastern 21 ICARIA Crater Hellas CIM MERIA SIRENUM PLANUM A ONI A TERRA PL ANIT I A Copernicus TERRA PR OMETHEI 29 ARG YRE TERRA –50° Crater –50° PL ANI T I A –57° –57° 180° E 210° E 240° E 270° E 300° E 330° E 0° E 30° E 60° E 90° E 120° E 150° E 180° E Exploration Zones proposed for humans to Mars. Prepared By: Lindsay Hays, Mars Program Office 00 Numbers correspond to the abstract submission # version 10.0 October 1, 2015 At the equator, circles are ~100km radius [email protected].

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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.
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Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identiﬁed in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km.
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RSL), Described in the 5 August 2011 Science Report “Seasonal Flows on Warm Martian Slopes”
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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.
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Arecibo Radar Imaging of Mars During the 2005 Opposition
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Lick Observatory Records: Photographs UA.036.Ser.07
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Solar Wind Charge Exchange X-Ray Emission from Mars. Dimitra Koutroumpa, Ronan Modolo, Gérard Chanteur, Jean-Yves Chaufray, V
Solar wind charge exchange X-ray emission from Mars. Dimitra Koutroumpa, Ronan Modolo, Gérard Chanteur, Jean-Yves Chaufray, V. Kharchenko, Rosine Lallement To cite this version: Dimitra Koutroumpa, Ronan Modolo, Gérard Chanteur, Jean-Yves Chaufray, V. Kharchenko, et al.. Solar wind charge exchange X-ray emission from Mars.: Model and data comparison. Astronomy and Astrophysics - A&A, EDP Sciences, 2012, 545, pp.A153. 10.1051/0004-6361/201219720. hal- 00731069 HAL Id: hal-00731069 https://hal.archives-ouvertes.fr/hal-00731069 Submitted on 2 Sep 2020 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. A&A 545, A153 (2012) Astronomy DOI: 10.1051/0004-6361/201219720 & c ESO 2012 Astrophysics Solar wind charge exchange X-ray emission from Mars Model and data comparison D. Koutroumpa1, R. Modolo1, G. Chanteur2, J.-Y., Chaufray1, V. Kharchenko3, and R. Lallement4 1 Université Versailles St-Quentin, CNRS/INSU, LATMOS-IPSL, 11 Bd d’Alembert, 78280 Guyancourt, France e-mail: [email protected] 2 Laboratoire de Physique des Plasmas, École Polytechnique, UPMC, CNRS, Palaiseau, France 3 Physics Department, University of Connecticut, Storrs, Connecticut, USA 4 GEPI, Observatoire de Paris, CNRS, 92195 Meudon, France Received 30 May 2012 / Accepted 17 August 2012 ABSTRACT Aims.
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1 Fluids Mobilization in Arabia Terra, Mars
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Large Impact Crater Histories of Mars: the Effect of Different Model Crater Age Techniques ⇑ Stuart J
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