Human Mars Landing Site and Impacts on Mars Surface Operations Ben Bussey Stephen J
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MODELED CATASTROPHIC OUTFLOW at ARAM CHAOS CHANNEL, MARS. DA Howard, Earth & Planetary Sciences, University of Tennessee
40th Lunar and Planetary Science Conference (2009) 2179.pdf MODELED CATASTROPHIC OUTFLOW AT ARAM CHAOS CHANNEL, MARS. D. A. Howard, Earth & Planetary Sciences, University of Tennessee, 306 Earth & Planetary Sciences Bldg., 1412 Circle Drive, Knoxville, TN 37996, [email protected]. Introduction: The Aram Chaos channel located at tional algorithms relied on in this study were devel- 2.8°N, 18.5°W, is approximately 100 km long, ranges oped by Komar [1] and I have adapted them for use from 8 to 14 km wide, and has a maximum depth of with the Hydrologic Engineering Center’s River Anal- 2000 m (Figure 1). The confined innermost approx- ysis System (HEC-RAS) based on solution of the con- imately 67 km reach selected for this study includes tinuity and momentum equations [2]. HEC-RAS ad- the area of the channel where the trimline is evident justed for Mars’ gravitational acceleration was only for the stream head at the time of initial catastrophic applied to Mars channels once previously by Burr [3] flow and the outflow height at the channel’s mouth. at Athabasca Vallis and therefore provides the oppor- tunity to further develop the method here. The HEC- RAS model used for both Earth and Mars are identical except that the Mars version was adjusted for the gra- vitational acceleration and the specific weight of water differences between the two planets. Using the HEC- Ares Valles GeoRAS ArcGIS geospatial tool to generate the chan- nel geometry for input to the HEC-RAS flow model, Aram Chaos the hypothesized output potentially quantifies the hy- draulics of the channels more accurately than previous orders-of-magnitude estimates reported in the litera- ture. -
Mars Water In-Situ Resource Utilization (ISRU) Planning (M-WIP) Study
Mars Water In-Situ Resource Utilization (ISRU) Planning (M-WIP) Study April 22, 2016 Angel Abbud-Madrid, David Beaty, Dale Boucher, Ben Bussey, Richard Davis, Leslie Gertsch, Lindsay Hays, Julie Kleinhenz, Michael Meyer, Michael Moats, Robert Mueller, Aaron Paz, Nantel Suzuki, Paul van Susante, Charles Whetsel, Elizabeth Zbinden (affiliations in Appendix) This “first-order” analysis of questions about supply-side planning related to potential water resource deposits on Mars was jointly requested by NASA-SMD and NASA-HEOMD in Jan. 2016. Recommended Bibliographic Citation: Abbud-Madrid, A., D.W. Beaty, D. Boucher, B. Bussey, R. Davis, L. Gertsch, L.E. Hays, J. Kleinhenz, M.A. Meyer, M. Moats, R.P. Mueller, A. Paz, N. Suzuki, P. van Susante, C. Whetsel, E.A. Zbinden, 2016, Report of the Mars Water In-Situ Resource Utilization (ISRU) Planning (M-WIP) Study; 90 p, posted April, 2016 at http://mepag.nasa.gov/reports/Mars_Water_ISRU_Study.pptx Copyright 2016 California Institute of Technology. U.S. Government sponsorship acknowledged. All rights reserved. Executive Summary (1 of 2) This scoping analysis is intended to provide guidance regarding a number of complex and inter- related issues involving the potential use of Martian water resources, and for which follow-up action by a number of different entities would be beneficial. • Objectives: 1). Formulate descriptions of hypothetical reserves on Mars, 2). Estimate the rough order-of-magnitude of the engineered system needed to produce each of the reference cases, 3). Prepare a first draft analysis of the sensitivity of the production system to the known or potential geological variation, 4). Prepare an initial description of the preliminary implications for exploration. -
A New Model of the Crustal Magnetic Field of Mars Using MGS and MAVEN
RESEARCH ARTICLE A New Model of the Crustal Magnetic Field of Mars Using 10.1029/2018JE005854 MGS and MAVEN Key Points: 1 1 2 3 • MGS and MAVEN magnetic field Benoit Langlais , Erwan Thébault , Aymeric Houliez , Michael E. Purucker , 4 measurements are combined into a and Robert J. Lillis high-resolution magnetic field model • The new model extends up to SH 1Laboratoire de Planétologie et Géodynamique, Université de Nantes, Université d'Angers, CNRS, UMR 6112, Nantes, degree 134, corresponding to 160-km France, 2Observatoire Royal de Belgique, Uccle, Belgium, 3Planetary Magnetospheres Laboratory, NASA Goddard horizontal resolution at the Martian Space Flight Center, Greenbelt, MD, USA, 4Space Science Laboratory, University of California, Berkeley, CA, USA surface • It enables local studies, where geologic and magnetic features can be compared Abstract While devoid of an active magnetic dynamo field today, Mars possesses a remanent magnetic field that may reach several thousand nanoteslas locally. The exact origin and the events that have shaped the crustal magnetization remain largely enigmatic. Three magnetic field data sets from two spacecraft Supporting Information: • Supporting Information S1 collected over 13 cumulative years have sampled the Martian magnetic field over a range of altitudes •TableS1 from 90 up to 6,000 km: (a) Mars Global Surveyor (MGS) magnetometer (1997–2006), (b) MGS Electron Reflectometer (1999–2006), and (c) Mars Atmosphere and Volatile EvolutioN (MAVEN) magnetometer Correspondence to: (2014 to today). In this paper we combine these complementary data sets for the first time to build a new B. Langlais, model of the Martian internal magnetic field. This new model improves upon previous ones in several [email protected] aspects: comprehensive data coverage, refined data selection scheme, modified modeling scheme, discrete-to-continuous transformation of the model, and increased model resolution. -
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, -
Impact Melt Emplacement on Mercury
Western University Scholarship@Western Electronic Thesis and Dissertation Repository 7-24-2018 2:00 PM Impact Melt Emplacement on Mercury Jeffrey Daniels The University of Western Ontario Supervisor Neish, Catherine D. The University of Western Ontario Graduate Program in Geology A thesis submitted in partial fulfillment of the equirr ements for the degree in Master of Science © Jeffrey Daniels 2018 Follow this and additional works at: https://ir.lib.uwo.ca/etd Part of the Geology Commons, Physical Processes Commons, and the The Sun and the Solar System Commons Recommended Citation Daniels, Jeffrey, "Impact Melt Emplacement on Mercury" (2018). Electronic Thesis and Dissertation Repository. 5657. https://ir.lib.uwo.ca/etd/5657 This Dissertation/Thesis is brought to you for free and open access by Scholarship@Western. It has been accepted for inclusion in Electronic Thesis and Dissertation Repository by an authorized administrator of Scholarship@Western. For more information, please contact [email protected]. Abstract Impact cratering is an abrupt, spectacular process that occurs on any world with a solid surface. On Earth, these craters are easily eroded or destroyed through endogenic processes. The Moon and Mercury, however, lack a significant atmosphere, meaning craters on these worlds remain intact longer, geologically. In this thesis, remote-sensing techniques were used to investigate impact melt emplacement about Mercury’s fresh, complex craters. For complex lunar craters, impact melt is preferentially ejected from the lowest rim elevation, implying topographic control. On Venus, impact melt is preferentially ejected downrange from the impact site, implying impactor-direction control. Mercury, despite its heavily-cratered surface, trends more like Venus than like the Moon. -
LAYERED SULFATE-BEARING TERRAINS on MARS: INSIGHTS from GALE CRATER and MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S
Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6316.pdf LAYERED SULFATE-BEARING TERRAINS ON MARS: INSIGHTS FROM GALE CRATER AND MERIDIANI PLANUM. K.E. Powell1,2, R.E. Arvidson3, and C.S. Edwards1, 1Department of Physics & Astrono- my, Northern Arizona University, 2School of Earth & Space Exploration, Arizona State University, 3Department of Earth & Planetary Sciences, Washington University in St. Louis. Introduction: Sulfate species have been detected ronment, with episodes of diagenesis and weathering in late Noachian and Hesperian terrains on Mars lying to form a crystalline hematite lag deposit [4, 5]. The stratigraphically above clay minerals, which has been lag deposit masks the CRISM spectral signature of interpreted as documenting a shift from wetter to more sulfate in most locations. Sulfate minerals including arid environments on the surface. Sulfate detections kieserite and gypsum have been detected in impact are associated with layered deposits in numerous loca- crater walls and windswept regions [6]. The Oppor- tions including Gale Crater, Meridiani Planum, Vallis tunity rover explored southern Meridiani Planum Marineris, and Terra Sirenum, and Aram Chaos [1]. through a campaign of crater-hopping, using craters as These sulfates and clays been identified using their a natural drill to expose strata [6]. The deepest expo- diagnostic absorption features in visible and near- sures explored by Opportunity directly are ~10 meters infrared reflectance (VNIR) data acquired from Mars thick at Victoria Crater. Opportunity results indicate orbit. Additionally, two rover missions have explored that the top layers of Burns formation contain up to sites with massive sulfate deposits. The first, the MER 40% sulfate and included Mg, Ca, and Fe species. -
MIAMI UNIVERSITY the Graduate School Certificate for Approving The
MIAMI UNIVERSITY The Graduate School Certificate for Approving the Dissertation We hereby approve the Dissertation of Qiuyuan Huang Candidate for the Degree: Doctor of Philosophy _______________________________________ Hailiang Dong, Director ________________________________________ Yildirim Dilek, Reader ________________________________________ Jonathan Levy, Reader ______________________________________ Chuanlun Zhang, External examiner ______________________________________ Annette Bollmann, Graduate School Representative ABSTRACT GEOMICROBIAL INVESTIGATIONS ON EXTREME ENVIRONMENTS: LINKING GEOCHEMISTRY TO MICROBIAL ECOLOGY IN TERRESTRIAL HOT SPRINGS AND SALINE LAKES by Qiuyuan Huang Terrestrial hot springs and saline lakes represent two extreme environments for microbial life and constitute an important part of global ecosystems that affect the biogeochemical cycling of life-essential elements. Despite the advances in our understanding of microbial ecology in the past decade, important questions remain regarding the link between microbial diversity and geochemical factors under these extreme conditions. This dissertation first investigates a series of hot springs with wide ranges of temperature (26-92oC) and pH (3.72-8.2) from the Tibetan Plateau in China and the Philippines. Within each region, microbial diversity and geochemical conditions were studied using an integrated approach with 16S rRNA molecular phylogeny and a suite of geochemical analyses. In Tibetan springs, the microbial community was dominated by archaeal phylum Thaumarchaeota -
The Geology of Aram Chaos. Timothy D
Lunar and Planetary Science XXXIV (2003) 2046.pdf The Geology of Aram Chaos. Timothy D. Glotch1, and Philip R. Christensen1, 1Department of Geological Sciences, Arizona State University, Tempe, AZ 85287-6305 Introduction. The Thermal Emission Spectrometer wavelengths, THEMIS cannot detect the presence of (TES) instrument aboard the Mars Global Surveyor hematite. Three-band, decorrelation-stretched images (MGS) spacecraft located deposits of gray, crystalline can however, provide information about any hematite in Sinus Meridiani, Aram Chaos, and Valles additional mineralogical variability that may be Marineris [1-2]. Since the initial discovery, most present in the area. work has focused on the Sinus Meridiani site, Individual MOLA tracks were used to characterize primarily because of its large size and its probable the regional sloping and tilting occurring within the choice as a landing site for one of NASA’s 2003 crater. In addition to the individual tracks, a 100- Mars Excursion Rover (MER) rovers [3-5]. meter contour map created from the 128 ppd gridded Christensen et al., [1-2] provided five testable data set was overlayed onto a THEMIS daytime hypotheses regarding the formation of crystalline mosaic to understand regional topographic trends. hematite on Mars: 1) low-temperature precipitaion of Results and Discussion. The topmost stratigraphic Fe oxides/hydroxides from standing, oxygenated, Fe- unit in Aram Chaos covers roughly 20% of the rich water, followed by subsequent alteration to gray interior of Aram Chaos. It is unique among the units hematite, 2) low-temperature leaching of iron-bearing in Aram Chaos in that it has a relatively high thermal silicates and other materials leaving a Fe-rich residue inertia (550-700 J/m2Ks1/2), indicating a layer (laterite-style weathering) which is subsequently composed of sand and pebble-sized particles [6], or altered to gray hematite, 3) direct precipitation of alternatively, smaller particles cemented together. -
Mineralogy of the Martian Surface
EA42CH14-Ehlmann ARI 30 April 2014 7:21 Mineralogy of the Martian Surface Bethany L. Ehlmann1,2 and Christopher S. Edwards1 1Division of Geological & Planetary Sciences, California Institute of Technology, Pasadena, California 91125; email: [email protected], [email protected] 2Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 Annu. Rev. Earth Planet. Sci. 2014. 42:291–315 Keywords First published online as a Review in Advance on Mars, composition, mineralogy, infrared spectroscopy, igneous processes, February 21, 2014 aqueous alteration The Annual Review of Earth and Planetary Sciences is online at earth.annualreviews.org Abstract This article’s doi: The past fifteen years of orbital infrared spectroscopy and in situ exploration 10.1146/annurev-earth-060313-055024 have led to a new understanding of the composition and history of Mars. Copyright c 2014 by Annual Reviews. Globally, Mars has a basaltic upper crust with regionally variable quanti- by California Institute of Technology on 06/09/14. For personal use only. All rights reserved ties of plagioclase, pyroxene, and olivine associated with distinctive terrains. Enrichments in olivine (>20%) are found around the largest basins and Annu. Rev. Earth Planet. Sci. 2014.42:291-315. Downloaded from www.annualreviews.org within late Noachian–early Hesperian lavas. Alkali volcanics are also locally present, pointing to regional differences in igneous processes. Many ma- terials from ancient Mars bear the mineralogic fingerprints of interaction with water. Clay minerals, found in exposures of Noachian crust across the globe, preserve widespread evidence for early weathering, hydrothermal, and diagenetic aqueous environments. Noachian and Hesperian sediments include paleolake deposits with clays, carbonates, sulfates, and chlorides that are more localized in extent. -
The Curtis L. Ivey Science Center DEDICATED SEPTEMBER 17, 2004
NON-PROFIT Office of Advancement ORGANIZATION ALUMNI MAGAZINE COLBY-SAWYER Colby-Sawyer College U.S. POSTAGE 541 Main Street PAID New London, NH 03257 LEWISTON, ME PERMIT 82 C LBY-SAWYER CHANGE SERVICE REQUESTED ALUMNI MAGAZINE I NSIDE: FALL/WINTER 2004 The Curtis L. Ivey Science Center DEDICATED SEPTEMBER 17, 2004 F ALL/WINTER 2004 Annual Report Issue EDITOR BOARD OF TRUSTEES David R. Morcom Anne Winton Black ’73, ’75 CLASS NOTES EDITORS Chair Tracey Austin Ye ar of Gaye LaCasce Philip H. Jordan Jr. Vice-Chair CONTRIBUTING WRITERS Tracey Austin Robin L. Mead ’72 the Arts Jeremiah Chila ’04 Executive Secretary Cathy DeShano Ye ar of Nicole Eaton ’06 William S. Berger Donald A. Hasseltine Pamela Stanley Bright ’61 Adam S. Kamras Alice W. Brown Gaye LaCasce Lo-Yi Chan his month marks the launch of the Year of the Arts, a David R. Morcom Timothy C. Coughlin P’00 Tmultifaceted initiative that will bring arts faculty members to meet Kimberly Swick Slover Peter D. Danforth P’83, ’84, GP’02 the Arts Leslie Wright Dow ’57 with groups of alumni and friends around the country. We will host VICE PRESIDENT FOR ADVANCEMENT Stephen W. Ensign gatherings in art museums and galleries in a variety of cities, and Donald A. Hasseltine Eleanor Morrison Goldthwait ’51 are looking forward to engaging hundreds of alumni and friends in Suzanne Simons Hammond ’66 conversations about art, which will be led by our faculty experts. DIRECTOR OF DEVELOPMENT Patricia Driggs Kelsey We also look forward to sharing information about Colby-Sawyer’s Beth Cahill Joyce Juskalian Kolligian ’55 robust arts curriculum. -
Meteorites on Ice
PSRD: Antarctic Meteorites http://www.psrd.hawaii.edu/Nov01/metsOnIce.html posted November 7, 2001 Meteorites on Ice --- Antarctic meteorites provide a continuous and readily available supply of extraterrestrial materials, stimulating new research and ideas in cosmochemistry, planetary geology, astronomy, and astrobiology. Written by Linda M.V. Martel Hawai'i Institute of Geophysics and Planetology Annual collections of meteorites from Antarctica are a steady source of new non-microscopic extraterrestrial material including lunar and Martian samples and rare and unusual flotsam from asteroids. This article summarizes research on new kinds of Antarctic meteorites that is not simply changing how meteorites are classified but causing a revolution in our knowledge of the materials and processes in the solar nebula, our solar system, and the formation of asteroids, planets, and ultimately our world. When the 2001-2002 Antarctic Search for Meteorites (ANSMET) field party begins scouting for meteorites on the ice this season, we will be continuing a 25-year tradition of exploration along the Transantarctic Mountains. As a new ANSMET meteorite hunter, I will report to PSRD on this season's search and recovery of specimens and how studies of Antarctic meteorites are unraveling the secrets of solar system formation. Reference: U. S. Antarctic Search for Meteorites program. Finding Rocks That Fall From Outer Space The U. S. Antarctic Search for Meteorites (ANSMET) program is a collaborative effort of the National Science Foundation (NSF), NASA, and the Smithsonian Institution. Field collection is supported currently by a grant from the NSF Office of Polar Programs to Principal Investigator Dr. Ralph Harvey at Case Western Reserve University in Cleveland, Ohio. -
Cambridge University Press 978-1-107-03629-1 — the Atlas of Mars Kenneth S
Cambridge University Press 978-1-107-03629-1 — The Atlas of Mars Kenneth S. Coles, Kenneth L. Tanaka, Philip R. Christensen Index More Information Index Note: page numbers in italic indicates figures or tables Acheron Fossae 76, 76–77 cuesta 167, 169 Hadriacus Cavi 183 orbit 1 Acidalia Mensa 86, 87 Curiosity 9, 32, 62, 195 Hadriacus Palus 183, 184–185 surface gravity 1, 13 aeolian, See wind; dunes Cyane Catena 82 Hecates Tholus 102, 103 Mars 3 spacecraft 6, 201–202 Aeolis Dorsa 197 Hellas 30, 30, 53 Mars Atmosphere and Volatile Evolution (MAVEN) 9 Aeolis Mons, See Mount Sharp Dao Vallis 227 Hellas Montes 225 Mars Chart 1 Alba Mons 80, 81 datum (zero elevation) 2 Hellas Planitia 220, 220, 226, 227 Mars Exploration Rovers (MER), See Spirit, Opportunity albedo 4, 5,6,10, 56, 139 deformation 220, See also contraction, extension, faults, hematite 61, 130, 173 Mars Express 9 alluvial deposits 62, 195, 197, See also fluvial deposits grabens spherules 61,61 Mars Global Surveyor (MGS) 9 Amazonian Period, history of 50–51, 59 Deimos 62, 246, 246 Henry crater 135, 135 Mars Odyssey (MO) 9 Amenthes Planum 143, 143 deltas 174, 175, 195 Herschel crater 188, 189 Mars Orbiter Mission (MOM) 9 Apollinaris Mons 195, 195 dikes, igneous 82, 105, 155 Hesperia Planum 188–189 Mars Pathfinder 9, 31, 36, 60,60 Aram Chaos 130, 131 domical mound 135, 182, 195 Hesperian Period, history of 50, 188 Mars Reconnaissance Orbiter (MRO) 9 Ares Vallis 129, 130 Dorsa Argentea 239, 240 Huygens crater 183, 185 massif 182, 224 Argyre Planitia 213 dunes 56, 57,69–70, 71, 168, 185,