Thermal Design of the Sample Handling Assembly in the Sampling and Caching Subsystem on the Mars 2020 Rover
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Imaginative Geographies of Mars: the Science and Significance of the Red Planet, 1877 - 1910
Copyright by Kristina Maria Doyle Lane 2006 The Dissertation Committee for Kristina Maria Doyle Lane Certifies that this is the approved version of the following dissertation: IMAGINATIVE GEOGRAPHIES OF MARS: THE SCIENCE AND SIGNIFICANCE OF THE RED PLANET, 1877 - 1910 Committee: Ian R. Manners, Supervisor Kelley A. Crews-Meyer Diana K. Davis Roger Hart Steven D. Hoelscher Imaginative Geographies of Mars: The Science and Significance of the Red Planet, 1877 - 1910 by Kristina Maria Doyle Lane, B.A.; M.S.C.R.P. Dissertation Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy The University of Texas at Austin August 2006 Dedication This dissertation is dedicated to Magdalena Maria Kost, who probably never would have understood why it had to be written and certainly would not have wanted to read it, but who would have been very proud nonetheless. Acknowledgments This dissertation would have been impossible without the assistance of many extremely capable and accommodating professionals. For patiently guiding me in the early research phases and then responding to countless followup email messages, I would like to thank Antoinette Beiser and Marty Hecht of the Lowell Observatory Library and Archives at Flagstaff. For introducing me to the many treasures held deep underground in our nation’s capital, I would like to thank Pam VanEe and Ed Redmond of the Geography and Map Division of the Library of Congress in Washington, D.C. For welcoming me during two brief but productive visits to the most beautiful library I have seen, I thank Brenda Corbin and Gregory Shelton of the U.S. -
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. -
Columbus Crater HLS2 Hangout: Exploration Zone Briefing
Columbus Crater HLS2 Hangout: Exploration Zone Briefing Kennda Lynch1,2, Angela Dapremont2, Lauren Kimbrough2, Alex Sessa2, and James Wray2 1Lunar and Planetary Institute/Universities Space Research Association 2Georgia Institute of Technology Columbus Crater: An Overview • Groundwater-fed paleolake located in northwest region of Terra Sirenum • ~110 km in diameter • Diversity of Noachian & Hesperian aged deposits and outcrops • High diversity of aqueous mineral deposits • Estimated 1.5 km depth of sedimentary and/or volcanic infill • High Habitability and Biosignature Preservation Potential LZ & Field Station Latitude: 194.0194 E Longitude: 29.2058 S Altitude: +910 m SROI #1 RROI #1 LZ/HZ SROI #4 SROI #2 SROI #5 22 KM HiRISE Digital Terrain Model (DTM) • HiRISE DTMs are made from two images of the same area on the ground, taken from different look angles (known as a stereo-pair) • DTM’s are powerful research tools that allow researchers to take terrain measurements and model geological processes • For our traversability analysis of Columbus: • The HiRISE DTM was processed and completed by the University of Arizona HiRISE Operations Center. • DTM data were imported into ArcMap 10.5 software and traverses were acquired and analyzed using the 3D analyst tool. • A slope map was created in ArcMap to assess slope values along traverses as a supplement to topography observations. Slope should be ≤30°to meet human mission requirements. Conclusions Traversability • 9 out of the 17 traverses analyzed met the slope criteria for human missions. • This region of Columbus Crater is traversable and allows access to regions of astrobiological interest. It is also a possible access point to other regions of Terra Sirenum. -
Downselection of Landing Sites Proposed for the Mars 2020 Rover Mission
47th Lunar and Planetary Science Conference (2016) 2324.pdf DOWNSELECTION OF LANDING SITES PROPOSED FOR THE MARS 2020 ROVER MISSION. M. P. Golombek1, J. A. Grant2, K. A. Farley3, K. Williford1, A. Chen1, R. E. Otero1, and J. W. Ashley1, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109; 2Smithsonian Institution, Center for Earth and Planetary Sciences, Washington, D.C. 20560, 3Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125. Introduction: The Mars 2020 mission would ex- suitable for addressing key planetary evolution ques- plore a site likely to have been habitable, seek signs of tions if and when they are returned to Earth. past life, prepare a returnable cache with the most Results of the voting were presented as the compelling samples, take the first steps towards in-situ weighted average (assigning 5 points to each green resource utilization on Mars, and demonstrate technol- vote, 3 to each yellow vote, and 1 to each red vote that ogy needed for future human and robotic exploration were then summed and divided by the total number of of Mars. The first landing site workshop identified and votes) and the mode (color receiving the most votes). prioritized 27 landing sites proposed by the science This ensured that participants could not skew the re- community according to science objectives that also sults by withholding votes from some sites. Both met the engineering constraints [1]. This abstract de- methods yield similar results and reveal a fall-off in scribes the downselection of landing sites that occurred support for sites ranked lower than the top nine or ten at the second landing site workshop and associated based on mode and average, respectively [2]. -
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. -
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. -
Downselection of Landing Sites for the Mars Science Laboratory
Lunar and Planetary Science XXXIX (2008) 2181.pdf DOWNSELECTION OF LANDING SITES FOR THE MARS SCIENCE LABORATORY. M. Golombek1, J. Grant2, A. R. Vasavada1, M. Watkins1, E. Noe Dobrea1, J. Griffes2, and T. Parker1, 1Jet Propulsion Laboratory, Cali- fornia Institute of Technology, Pasadena, CA 91109, 2Smithsonian Institution, National Air and Space Museum, Center for Earth and Planetary Sciences, Washington, D.C. 20560. Introduction: Six landing sites remain under con- 3°E), Terby crater (28°S, 74°E), Melas Chasma (10°S, sideration for the Mars Science Laboratory (MSL) 284°E), E Meridiani (0°N, 4°E), and Miyamoto crater after discussion of over 30 general sites at the Second (referred to as Runcorn crater or E and S Meridiani at Landing Site Workshop and a subsequent project meet- the workshop) (3°S, 353°E). ing. This abstract discusses the downselection process, Additional discussion that included consideration defines the sites under consideration and describes of engineering constraints and science diversity further subsequent activities to select the final landing site. trimmed the list to six: Nili Fossae trough, Holden cra- Second Landing Site Workshop: After the First ter, Mawrth Vallis, Jezero crater, Terby crater, and Landing Site Workshop in June 2006, 33 general land- Miyamoto crater. Four sites from the top eleven that ing sites that incorporated 94 landing ellipses (multiple did not make the final list, but might satisfy the engi- ellipses were proposed for some sites) [1] were tar- neering constraints include Eberswalde, NE Syrtis, geted with Mars Reconnaissance Orbiter (MRO), Mars Chloride sites, and E Meridiani. These four sites were Odessey, and Mars Global Surveyor observations. -
Holden Crater
M2020 Candidate Landing Site Data Sheets HOLDEN CRATER Location 325.11E, 26.62S Holden Crater (lat,lon): Summary of observations and interpreted history, including unknowns: Holden Crater impacted into the pre-existing Uzboi-Ladon-Marova regional drainage system either in the Late Noachian (Grant et al 2008) or as late as the Late Hesperian (3.58Gy; N. Mangold, personal communication), most likely after the main era of ULM activity. For some period starting after the impact, precipitation and runoff from the crater walls or perhaps groundwater partially filled the crater with a lake, depositing a series of clay-bearing light-toned layered deposits (lower unit, lower member). Perhaps mirroring the overall drying of Mars during the Hesperian, or alternatively due to tailing off of local impact- induced precipitation, the crater lake gradually dried out over time (lower unit, middle member), perhaps going through one or more playa phases, and eventually transitioning into a much drier, alluvium- dominated system (lower unit, upper member). The alluvial phase was largely terminated by a major flood event that breached the rim at the location of the pre-existing Uzboi Vallis and deposited dark and coarse flood deposits in the region of the ellipse (upper unit) and more finely layered lacustrine facies toward the center of the crater. The flood event may have created a (transient?) lake up to 250 meters deep. Since this time, Holden has experienced minimal alluvial and significant aeolian activity. Subsequent cratering and erosion has exposed underlying clay and silica-bearing megabreccia blocks formed during or prior to the Holden Crater impact, which may preserve an ancient impact hydrothermal system. -
Eberswalde Crater
M2020 Candidate Landing Site Data Sheets Eberswalde crater Location 23.8S, 326.7E Eberswalde Crater (lat,lon): Summary of observations and interpreted history, including unknowns: Eberswalde crater (first identified as “NE Holden crater” in 2003 by Malin and Edgett) contains a 10 km * 10 km fan structure interpreted by the large majority of the published works as a delta. The delta is up to 100 m thick and shows sinuous, locally meandering channels preserved from erosion and appearing in inverted relief. Sediments at the front of the delta contain clay minerals and are eroded by wind with well-exposed, fresh outcrops of clastic deposits. Opaline silica has also been detected in the deltaic deposits and other crater floor materials. The timing of the fluvial activity is constrained by the presence of Holden ejecta that are incised by the channels leading to the delta, and by the onlapping of delta sediments onto Holden ejecta deposits within Eberswalde crater. The crosscutting relationships show that Eberswalde delta formed later than Eberswalde crater itself, and after Holden crater, which is dated Early Hesperian. The TRN ellipse contains deltaic deposits in addition to the paleolake bottom. The material covering the Eberswalde crater floor is diverse, and it may contain local exposures of lakebeds. The ellipse also contains other units including pitted material of unclear origin, megabreccia that may correspond to Holden impact ejecta, and large veins. Origin of the vein-fill is also uncertain, although igneous processes and hydrothermalism have been proposed. The site does not show any clear evidence for in-place igneous rocks. -
Timing, Duration, and Hydrology of the Eberswalde Crater Paleolake, Mars
42nd Lunar and Planetary Science Conference (2011) 2748.pdf TIMING, DURATION, AND HYDROLOGY OF THE EBERSWALDE CRATER PALEOLAKE, MARS. R. P. Irwin III, Planetary Science Institute, 1700 E. Fort Lowell Rd., Suite 106, Tucson AZ 85719, [email protected], visiting scientist at NASA Goddard Space Flight Center, Code 698, Greenbelt MD 20771. Introduction: Martian paleolakes offer a conve- the southern one are 140 and 180 m3/s using equations nient setting for mass- and energy-balance calculations 1 and 2, respectively. These results are broadly con- to constrain the past hydrology and water source [1,2]. sistent with previous studies [4,15,16]. Eberswalde crater is particularly useful in this regard due to its relict delta [3–7] that reflects the water level in the crater. Here we use the dominant discharge es- timated from inverted-channel width and meander geometry, the area of the paleolake and contributing watershed, and energy requirements for lake evapora- tion to constrain the mean annual runoff production and water source. Given the maximum age of the delta based on crater counts on Holden ejecta [8], these re- sults suggest a discrete post-Noachian interval of fluvial erosion on Mars. Age of the Eberswalde Delta: Although Ebers- walde crater is older than the adjacent Holden crater, the Eberswalde delta post-dates the Holden impact and superimposes its ejecta [4,8], which provide a larger surface area for crater counts. The superimposed cra- ter population >1 km in diameter indicates a Late Hes- perian age for Holden crater, with error bars that range within the Early and Late Hesperian Epochs [8]. -
Wind-Driven Erosion and Exposure Potential at Mars 2020 Rover
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Wind-Driven Erosion and Exposure Potential 10.1002/2017JE005460 at Mars 2020 Rover Candidate-Landing Sites Special Section: Matthew Chojnacki1 , Maria Banks2 , and Anna Urso1 5th International Planetary Dunes Workshop Special Issue 1Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA, 2NASA Goddard Space Flight Center, Greenbelt, MD, USA Key Points: • Candidate-landing sites for the Mars ’ 2020 Rover mission were assessed for Abstract Aeolian processes have likely been the predominant geomorphic agent for most of Mars history potential erosion by active eolian and have the potential to produce relatively young exposure ages for geologic units. Thus, identifying local bedforms evidence for aeolian erosion is highly relevant to the selection of landing sites for future missions, such as • Of the three downselected sites NE Syrtis then Jezero crater showed the the Mars 2020 Rover mission that aims to explore astrobiologically relevant ancient environments. Here we most evidence for ongoing sand investigate wind-driven activity at eight Mars 2020 candidate-landing sites to constrain erosion potential at transport and erosion potential these locations. To demonstrate our methods, we found that contemporary dune-derived abrasion rates • The Columbia Hills site lacked evidence for sand movement from were in agreement with rover-derived exhumation rates at Gale crater and could be employed elsewhere. local bedforms, suggesting that The Holden crater candidate site was interpreted to have low contemporary erosion rates, based on the current abrasion rates are low presence of a thick sand coverage of static ripples. Active ripples at the Eberswalde and southwest Melas sites may account for local erosion and the dearth of small craters. -
Stratigraphy in the Mawrth Vallis Region Through OMEGA, HRSC Color Imagery and DTM D
Stratigraphy in the Mawrth Vallis region through OMEGA, HRSC color imagery and DTM D. Loizeau, N. Mangold, F. Poulet, V. Ansan, E. Hauber, J.-P. Bibring, B. Gondet, Y. Langevin, P. Masson, G. Neukum To cite this version: D. Loizeau, N. Mangold, F. Poulet, V. Ansan, E. Hauber, et al.. Stratigraphy in the Mawrth Vallis region through OMEGA, HRSC color imagery and DTM. Icarus, Elsevier, 2010, 205 (2), pp.396. 10.1016/j.icarus.2009.04.018. hal-00612400 HAL Id: hal-00612400 https://hal.archives-ouvertes.fr/hal-00612400 Submitted on 29 Jul 2011 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. Accepted Manuscript Stratigraphy in the Mawrth Vallis region through OMEGA, HRSC color im‐ agery and DTM D. Loizeau, N. Mangold, F. Poulet, V. Ansan, E. Hauber, J.-P. Bibring, B. Gondet, Y. Langevin, P. Masson, G. Neukum PII: S0019-1035(09)00185-7 DOI: 10.1016/j.icarus.2009.04.018 Reference: YICAR 9015 To appear in: Icarus Received Date: 19 August 2008 Revised Date: 10 April 2009 Accepted Date: 14 April 2009 Please cite this article as: Loizeau, D., Mangold, N., Poulet, F., Ansan, V., Hauber, E., Bibring, J.-P., Gondet, B., Langevin, Y., Masson, P., Neukum, G., Stratigraphy in the Mawrth Vallis region through OMEGA, HRSC color imagery and DTM, Icarus (2009), doi: 10.1016/j.icarus.2009.04.018 This is a PDF file of an unedited manuscript that has been accepted for publication.