DOCSLIB.ORG

A Lake in Uzboi Vallis and Implications for Late Noachian Climate on Mars

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
A Lake in Uzboi Vallis and Implications for Late Noachian Climate on Mars 41st Lunar and Planetary Science Conference (2010) 1834.pdf A LAKE IN UZBOI VALLIS AND IMPLICATIONS FOR LATE NOACHIAN CLIMATE ON MARS. J. A. Grant1, D. Buczkowski2, R. P. Irwin, III1, and K. Siebach3, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, 6th St. at Independence Ave. SW, Washington, DC 20560, [email protected], 2Applied Physics Laboratory, Johns Hopkins University, 11100 John Hopkins Road, Laurel, MD 20723, 3Earth and Planetary Sciences, Washington University in Saint Louis, Saint Louis, MO 63130. Introduction: Uzboi Vallis (centered at ~28°S, The Uzboi Lake Basin: The Uzboi basin is deep- 323°E) is the southernmost segment of the northward- est and bounding relief is lowest where the Holden draining Uzboi-Ladon-Morava (ULM) meso-scale crater rim rises ~900 m above the floor to an elevation outflow system [1-3]. The ULM emerges from Argyre of –350 m (Fig. 1). Distributaries crossing the south- basin, and the associated catchment covers ~9% of west rim of Holden crater from Uzboi [9] indicate that Mars [4, 5]. Originally, the ULM consisted of incised flooding to this level created a lake of >4000 km3. segments draining radially across the structural rings of the Holden and Ladon impact basins [6] that were separated by depositional systems within the ancient basin centers [1]. Uzboi’s connection with Argyre was interrupted by the craters Bond and then Hale [7, 8], and drainage into Holden basin was blocked by Hol- den crater to the north, creating a ~400-km-long en- closed basin that was flooded during the late Noachian [9]. Figure 2. HiRISE image PSP_006189_1510_RED (25 cm pixel-scale) in Uzboi basin (28.8°S, 323.9°E). Here and elsewhere, smooth dark-toned deposits (upper left) rise to the –350 m contour and are interpreted as lacu- strine deposits. A transition to rougher surfaces occurs above –350 m. North is up. Additional evidence of impoundment in Uzboi is provided by thin, dark-toned deposits below –350 m (Fig. 2), layered deposits mostly exposed in alcoves, tributaries that terminate near –350 m, possible shore- lines, layered fill within an unnamed crater (Fig. 1) that is fractured into ~5–15 m polygons (Fig. 3), and local ponding in topographic lows of alluvium that is sometimes characterized by diverse, 50–100 m poly- gons. Once filled, Uzboi lake was geologically short- lived and drained rapidly into Holden crater. The common termination of most tributaries (except Nir- gal) at about –350 and absence of recognizable deposi- tional features where tributaries debouched into the Uzboi lake or at the limit of backflooding in Nirgal Vallis (Fig. 1) indicates lake level was not stable at lower elevations for a long period. Water overtopping Figure 1. MOLA topography over THEMIS daytime Holden’s rim coalesced into a dominant breach [9] that IR mosaic 2.0 of Uzboi Vallis/basin. Elevations range incised hundreds of meters as the lake drained into the from ~1300 m (red) to ~–2300 m (purple). The blue crater. Resultant fan deltas on the floor of Holden ex- within Uzboi Vallis is the area below –350 m, flooded tend more than 25 km from the breach and incorporate before the rim of Holden crater was overtopped. The meter-sized blocks whose transport requires high dis- rim of Bond crater was not overtopped, but lower Nir- charge. In addition, longitudinal grooves along the gal Vallis was backflooded. North is up. 41st Lunar and Planetary Science Conference (2010) 1834.pdf basin floor are hundreds of meters long and average 60 m, respectively, indicating that the regional water table m wide. These grooves, potholes, and other erosional was below the –1300 m floor of Uzboi. Nirgal Vallis is bedforms common to large floods on Earth suggest the major tributary to Uzboi, but it grades to the floor that they were formed by cavitation/macroturbulence of the basin, lacks depositional features associated [10–15] during rapid draining of at least the final stag- with backflooding, and shows little evidence for post- es of the Uzboi lake. On the Earth, similar longitudinal lake discharge [9]. Hence, while Nirgal Vallis may forms are associated with discharge rates of 105 to 106 have contributed discharge to the Uzboi lake, it likely m3/sec and flow velocities exceeding 10 m/s [10–15]. existed in something close to its present form prior to filling and draining of basin. Most Uzboi basin tributaries terminate at or near the –350-m contour and imply a base level near that elevation during much of their incision. These tributa- ries show poor connections with valley segments low- er in the basin that were likely reactivated or wholly formed during lake draining and subsequent draw- down of the local water table. Because tributaries above –350 m did not respond to lake draining and a dramatic lowering of base level (hundreds of meters), their incision must have ended when the lake drained. Implications: The Uzboi lake may have coincided with or just followed late Noachian alluvial and lacu- strine activity in Holden crater [9]. Little groundwater Figure 3. HiRISE image ESP_013586_1490_RGB (50 contribution to the Uzboi lake points to runoff from cm pixel-scale) of polygons disrupting layered fill in regional surfaces as the primary source of water and an unnamed crater inundated during flooding (Fig. 1). may require widespread precipitation. The absence of Comparison between the volume of water in the abrupt relief (outside of craters) or regional slopes that Uzboi lake and the lesser volume represented by the might induce orographic precipitation in Uzboi’s direct upper limit of benches, fan deltas, and lacustrine depo- watershed implies that precipitation was associated sits in Holden [9, 16] indicates that lake draining was with a broader, perhaps global, but short-lived and not a single event. Wall failures may have partly abruptly ending hydrologic system in the late Noa- dammed the breach during incision and led to pulsed chian [e.g., 17, 18]. discharge. Observed post-drainage slides into the References: [1] Grant J. A., and Parker, T. J. breach support this interpretation. (2002) JGR, 107, 10.1029/2001JE001678. [2] T. J. Limited CRISM data of the lake deposits and un- Parker (1985), thesis, California State University Pon- derlying basin floor (FRT0000ABB5) reveal Mg- drelli M. et al. (2005) JGR, 110, 2004JE002335. [3] smectites (possibly saponite or hectorite) that appear Saunders, S. R., (1979) USGS Map I-1144. [4] Ba- enriched in Fe in the basin floor (possibly a nontronite- nerdt, W.B. (2000), Eos Trans. AGU, 81, Abstract saponite mixture). CRISM data of the breach into Hol- #P52C-04 [5] Phillips, R.J., et al. (2001) Science, 291, den crater (HRS0001266E) confirm more outcrops of 2587–2591. [6] Schultz P. H. et al. (1982) JGR, 87, Mg-smectite-bearing rocks but also reveal a thin (tens 9803. [7] Philippoff, A.J., et al. (2009) LPSC XL, of meters thick) near-surface layer of possible Mg- 1737. [8] Reiss, D., et al. (2009) PSS, 57, 958-974, chlorite (clinochlore). The basin-floor smectites may doi:10.1016/j.pss.2008.09.008. [9] Grant, J. A., et al., reflect long-term weathering before the lake formed in (2008) Geology, 36, 195-198, doi: 10.1130/G24340A. Uzboi Vallis. The smectites in the lake deposits likely [10] Alho, P., et al. (2005) Quat. Sci. Rev., 24, 2319- reflect erosion and redeposition of these older smec- 2334. [11] Baker, V.R. (2001) Nature, 412, 228-236. tites, given that the lake was geologically short-lived. [12] Baker, V.R. (2002) Science, 295, 2379-2380. [13] The origin of Mg-chlorite near Holden’s rim is uncer- Baker, V.R. (2009) Ann. Rev. Earth and Planet. Sci., tain, but occurrence as a near-surface layer implies that 37, 393-411. [14] Baker, V., et al. (1988) Flood Geo- it post-dates crater formation and may be related to morphology: NY, Wiley Interscience, 503 p. [15] Gup- impact-induced or other post-crater alteration. ta, S., et al. (2007) Nature, 448, 342-346. [16] Pon- Source of Water: Regional groundwater contribu- drelli M. et al. (2005) JGR, 110, 2004JE002335. [17] tions to the Uzboi lake were likely minor, because al- Wray, J. J. et al. (2009) Geology, 37, 1043-1046, doi: luvial fans in adjacent Holden crater and Ostrov crater 10.1130/G30331A.1. [18] Irwin R. P. III et al. (2005), ~200 km east of Holden grade to –1900 m and –1500 JGR, 110, doi:10.1029/2005JE002460. .
Load more

Recommended publications
  • 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,
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • Mars, Past, Present, and Future
    MARS: PAST, PRESENT, AND FUTURE-RESULTS FROM THE MSATT PROGRAM MATT Mars Surface and Atmosphere Through Time LPI Technical Report Number 93-06, Part 1 Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPIITR--93-06, Part 1 MARS: PAST, PRESENT, AND FUTURE­ RESULTS FROM THE MSATT PROGRAM Edited by R. M. Haberle Convened by The MSAIT Steering Committee Held at Houston, Texas November 15-17, 1993 Sponsored by Mars Surface and Atmosphere Through Time (MSAIT) Study Group Lunar and Planetary Institute Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Technical Report Number 93-06, Part 1 LPIfTR--93-06, Part 1 Compiled in 1993 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the University Space Research Association under Contract No. NASW -4574 with the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication. This report may be cited as Haberle R. M., ed. (1993) Mars: Past Present, and Future-Results fr01ll the MSAIT Program. LPI Tech. Rpt. 93-06, Part 1. Lunar and Planetary Institute, Houston. 58 pp. This report is distributed by ORDER DEPARTMENT Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Mail order requestors will be invoiced for the cost of shipping alld halldling. [PI Technical Report 93-06. Part I iii Preface This volume contains papers that have been accepted for presentation at the workshop on Mars: Past, Present, and Future-Results from the MSAIT Program, November 15-17, 1993, in Houston, Texas.
    [Show full text]
  • Her Desher and Nirgal Vallis Phyllosilicates: Pedogenesis Or Groundwater Sapping?
    EPSC Abstracts Vol. 9, EPSC2014-523, 2014 European Planetary Science Congress 2014 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2014 Her Desher and Nirgal Vallis phyllosilicates: Pedogenesis or groundwater sapping? D. Buczkowski (1), S. Ackiss (1), K. Seelos (1), S. Murchie (1), F. Seelos (1), E. Malaret (2), and C. Hash (2). (1) Johns Hopkins University Applied Physics Laboratory, Maryland, USA, (2) Applied Coherent Technology, Virginia, USA ([email protected]) Abstract This distinct phyllosilicate-bearing layer is located only a few meters below the surface cap material and A widespread phyllosilicate-bearing layer has been is laterally contiguous with a uniform apparent identified in a distinct region in northwest Noachis thickness of ~10 meters. HiRISE observations of Terra [1,2,3]. This layer is exposed along the length these layers show the smectite-bearing materials to of two valley systems in the region, as well as crater be polygonally fractured, which is morphologically rims/walls. It has been suggested that the phyllosili- similar to other phyllosilicates identified on Mars [7]. cates were produced by pedogenic weathering fed by meteoric water or melted snow [2]. However, the geomorphology of the valley systems is consistent with formation due to groundwater sapping [4,5,6], opening the possibility that the phyllosilicates formed by interaction with groundwater, not surface water. 1. Introduction Noachis Terra is a highland cratered plain on Mars, extending from 20º to 80ºS latitude and 55ºW to 30ºE longitude. Two small valley systems incise NW Noachis Terra: Her Desher and Nirgal Valles (Fig. 1). Nirgal Vallis is a tributary of Uzboi Vallis, joining the larger system to the south of Holden Figure 1: MOLA topography draped over THEMIS crater.
    [Show full text]
  • The Argyre Region As a Prime Target for in Situ Astrobiological Exploration of Mars
    ASTROBIOLOGY Volume 16, Number 2, 2016 ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2015.1396 The Argyre Region as a Prime Target for in situ Astrobiological Exploration of Mars Alberto G. Faire´n,1,2 James M. Dohm,3 J. Alexis P. Rodrı´guez,4 Esther R. Uceda,5 Jeffrey Kargel,6 Richard Soare,7 H. James Cleaves,8,9 Dorothy Oehler,10 Dirk Schulze-Makuch,11,12 Elhoucine Essefi,13 Maria E. Banks,4,14 Goro Komatsu,15 Wolfgang Fink,16,17 Stuart Robbins,18 Jianguo Yan,19 Hideaki Miyamoto,3 Shigenori Maruyama,8 and Victor R. Baker6 Abstract At the time before *3.5 Ga that life originated and began to spread on Earth, Mars was a wetter and more geologically dynamic planet than it is today. The Argyre basin, in the southern cratered highlands of Mars, formed from a giant impact at *3.93 Ga, which generated an enormous basin approximately 1800 km in diameter. The early post-impact environment of the Argyre basin possibly contained many of the ingredients that are thought to be necessary for life: abundant and long-lived liquid water, biogenic elements, and energy sources, all of which would have supported a regional environment favorable for the origin and the persistence of life. We discuss the astrobiological significance of some landscape features and terrain types in the Argyre region that are promising and accessible sites for astrobiological exploration. These include (i) deposits related to the hydrothermal activity associated with the Argyre impact event, subsequent impacts, and those associated with the migration of heated water along Argyre-induced
    [Show full text]
  • Geologic Mapping in Margaritifer Terra on Mars and a Closer Look at the Confluence of Nirgal and Uzboi Valles
    47th Lunar and Planetary Science Conference (2016) 2505.pdf GEOLOGIC MAPPING IN MARGARITIFER TERRA ON MARS AND A CLOSER LOOK AT THE CONFLUENCE OF NIRGAL AND UZBOI VALLES. S. A. Wilson1 and J. A. Grant1, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, 6th at Independence SW, Washington, DC, USA ([email protected]). Introduction: Geologic mapping in Mars Trans- Hesperian Highland unit (Nh) is heavily cratered, dif- verse Mercator (MTM) quadrangles -20037, -25037, - ferentially mantled, contains older valley networks, 30037 and -30032 in southern Margaritifer Terra en- grabens, and a few wrinkle ridges. In the walls of compasses Uzboi Vallis and the terrain south and west Nirgal Vallis west of Uzboi, a ~10 m-thick, laterally of Holden and Ladon basins (Fig. 1). This region pre- continuous Fe/Mg-smectite phyllosilicate-bearing layer serves a long record of fluvial activity [e.g., 1-9] and is located a few meters below the surface of unit Nh mapping constrains the timing, source, duration and and stratigraphically above Al-phyllosilicates [13-14]. relative importance of aqueous and other geomorphic Evidence of this phyllosilicate layer east of Uzboi is processes in shaping the landscape. not observed [8]. The Late Noachian to Early Hesperi- an Terra unit (HNt) is characterized by widespread, smooth to rolling, cratered and variably dissected sur- faces between degraded impact craters [5]. Unit HNt in MTM -25037 occurs beneath continuous Holden ejecta (unit Hc2) and secondary craters related to the impact. The contact between units Nh and HNt are after [5]. Crater and Channel-Fill Units.
    [Show full text]
  • Eberswalde Delta in Margaritifer Terra
    PHASES OF EROSION AND DEPOSITION RECORDED IN HOLDEN CRATER OUTCROPS NOTE ADDED BY JPL WEBMASTER: This content has not been approved or adopted by, NASA, JPL, or the California Institute of Technology. This document is being made available for information purposes only, and any views and opinions expressed herein do not necessarily state or reflect those of NASA, JPL, or the California Institute of Technology. ROSS IRWIN1, JAMES WRAY2, AND JOHN GRANT1 1. SMITHSONIAN INSTITUTION, 2. GEORGIA TECH MARS GEOLOGIC EPOCHS Early Amazonian: 3.00-3.46 Ga Late Hesperian: Some late fluvial activity 3.40-3.65 Ga Early Hesperian: Valley networks, oldest 1-4 km craters 3.57-3.74 Ga Late Noachian: Cratering declines, basin infilling, small landforms eradicated 3.85-3.86 Ga Middle Noachian: Heavy bombardment, widespread highland resurfacing, Argyre 3.97-3.96 Ga: Isidis Early Noachian: Heavy bombardment, Hellas ? Pre-Noachian: Ages from Werner and Tanaka (2011) INTERCRATER PLAINS 100 km INTERCRATER PLAINS 100 km GLOBAL HIGHLAND UNIT CRATER POPULATIONS 1-4 km INTERCRATER PLAINS ON MERCURY INTERCRATER PLAINS ON MARS VALLEY NETWORKS AND PROMINENT DEPOSITS Hynek et al. (2010), JGR Wilson et al. (2013), LPSC REGIONAL CONTEXT U: Uzboi Vallis Ladon L: Ladon Valles M: Morava Valles h: Holden crater e: Eberswalde crater Holden o: Ostrov crater Ladon and Holden impact basin rings are dashed HOLDEN CRATER OVERVIEW . 26°S, 34°W . 155 km diam. –2 km floor . Phyllosilicate- rich LTL rocks . Alluvial fans and bajada from deeply dissected wall alcoves . Coarse flood deposit from Uzboi Vallis rim breach . Underlying bedrock outcrops 50 km 20 km 12 DISSECTED CRATERS SUPERIMPOSED ON HOLDEN Shown here See Grant and Wilson (2012) & Irwin et al., submitted D = 7 km D = 12 km 15 km FANS IN NORTHWEST HOLDEN CRATER 20 km EBERSWALDE LOBES Mosaic: Malin Space Science Systems Topographic Watershed -1350 m Dissected Watershed Internal Watershed -1400 m EBERSWALDE CRATER PALEOHYDROLOGY Width-wavelength relationships in two inverted paleochannels .
    [Show full text]
  • Early Mars Environments Revealed Through Near-Infrared Spectroscopy of Alteration Minerals
    Early Mars Environments Revealed Through Near-Infrared Spectroscopy of Alteration Minerals By Bethany List Ehlmann A.B., Washington University in St. Louis, 2004 M.Sc., University of Oxford, 2005 MSc. (by research), University of Oxford, 2007 Sc.M., Brown University, 2008 A dissertation Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Program in Geological Sciences at Brown University Providence, Rhode Island May 2010 i © Copyright 2010 Bethany L. Ehlmann ii Curriculum Vitae Bethany L. Ehlmann Dept. of Geological Sciences [email protected] Box 1846, Brown University (office) +1 401.863.3485 (mobile) +1 401.263.1690 Providence, RI 02906 USA EDUCATION Ph.D. Brown University, Planetary Sciences, anticipated May 2010 Advisor: Prof. John Mustard Sc. M., Brown University, Geological Sciences, 2008 Advisor: Prof. John Mustard M.Sc. by research, University of Oxford, Geography (Geomorphology), 2007 Advisor: Prof. Heather Viles M.Sc. with distinction, University of Oxford, Environmental Change & Management, 2005 Advisor: Dr. John Boardman A.B. summa cum laude, Washington University in St. Louis, 2004 Majors: Earth & Planetary Sciences, Environmental Studies; Minor: Mathematics Advisor: Prof. Raymond Arvidson International Baccalaureate Diploma, Rickards H.S., Tallahassee, Florida, 2000 Additional Training: Nordic/NASA Summer School: Water, Ice and the Origin of Life in the Universe, Iceland, July 2009 Vatican Observatory Summer School in Astronomy &Astrophysics, Castel Gandolfo, Italy,
    [Show full text]
  • NASA Scientific and Technical Aerospace Reports
    NASA STI Program ... in Profile Since its founding, NASA has been dedicated • CONFERENCE PUBLICATION. to the advancement of aeronautics and space Collected papers from scientific and science. The NASA scientific and technical technical conferences, symposia, information (STI) program plays a key part in seminars, or other meetings sponsored helping NASA maintain this important role. or co-sponsored by NASA. The NASA STI program operates under the • SPECIAL PUBLICATION. Scientific, auspices of the Agency Chief Information technical, or historical information from Officer. It collects, organizes, provides for NASA programs, projects, and missions, archiving, and disseminates NASA’s STI. The often concerned with subjects having NASA STI program provides access to the substantial public interest. NASA Aeronautics and Space Database and its public interface, the NASA Technical Report • TECHNICAL TRANSLATION. Server, thus providing one of the largest English-language translations of foreign collections of aeronautical and space science scientific and technical material pertinent to STI in the world. Results are published in both NASA’s mission. non-NASA channels and by NASA in the NASA STI Report Series, which includes the Specialized services also include organizing following report types: and publishing research results, distributing specialized research announcements and feeds, • TECHNICAL PUBLICATION. Reports of providing help desk and personal search completed research or a major significant support, and enabling data exchange services. phase of research that present the results of NASA Programs and include extensive data For more information about the NASA STI or theoretical analysis. Includes compila- program, see the following: tions of significant scientific and technical data and information deemed to be of • Access the NASA STI program home page continuing reference value.
    [Show full text]
  • (Hirise) During MRO's Primary Science Phase (PSP) Alfred S
    Icarus 205 (2010) 2-37 Contents lists available at ScienceDirect Icarus ELSEVIER journal homepage: www.elsevier.com/locate/icarus The High Resolution Imaging Science Experiment (HiRISE) during MRO's Primary Science Phase (PSP) Alfred S. McEwen3-*, Maria E. Banks3, Nicole Baugh3, Kris Beckerb, Aaron Boyd3, James W. Bergstromc, Ross A. Beyerd, Edward Bortolinic, Nathan T. Bridges6, Shane Byrne3, Bradford Castalia3, Frank C. Chuangf, Larry S. Grumpier ^, Ingrid Daubar3, Alix K. Davatzesh, Donald G. Deardorffd, Alaina Dejong3, W. Alan Delamere1, Eldar Noe Dobreae, Colin M. Dundas3, Eric M. Eliason3, Yisrael Espinoza3, Audrie Fennema3, Kathryn E. Fishbaughj, Terry Forrester3, Paul E. Geisslerb, John A. GrantJ, Jennifer L Griffes k, John P. Grotzingerk, Virginia C. Gulickd, Candice J. Hansen6, Kenneth E. Herkenhoffb, Rodney Heyd 3, Windy L Jaeger b, Dean Jones3, Bob Kanefsky d, Laszlo Keszthelyib, Robert King 3, Randolph L Kirkb, Kelly J. Kolb3, Jeffrey Lascoc, Alexandra Lefort1, Richard Leis3, Kevin W. Lewis k, Sara Martinez-Alonsom, Sarah Mattson3, Guy McArthur3, Michael T. Mellon•, Joannah M. Metzk, Moses P. Milazzob, Ralph E. Milliken6, Tahirih Motazedian3, Chris H. Okubob, Albert Ortiz3, Andrea J. Philippoff3, Joseph Plassmann3, Anjani Polit3, Patrick S. Russell1, Christian Schaller3, Mindi L Searlsm, Timothy Spriggs3, Steven W. Squyres", Steven Tarrc, Nicolas Thomas1, Bradley J. Thomson6,0, Livio L. Tornabene3, Charlie Van Houtenc, Circe Verbab, Catherine M. Weitzf, James J. Wray n "Lunar and Planetary Lab, University of Arizona, Tucson, AZ 85721, USA bU.S. Geological Survey, 2255 N. Gemini Drive, Flagstaff, AZ 86001, USA cBall Aerospace & Technologies Corp., 1600 Commerce St., Boulder, CO 80301, USA dNASA Ames Research Center and SETI Institute, Moffett Field, CA 94035, USA eJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA 'Planetary Science Institute, 1700 E.
    [Show full text]