DOCSLIB.ORG

MARS CRYOSPHERE 6:00 P.M

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
MARS CRYOSPHERE 6:00 P.M 45th Lunar and Planetary Science Conference (2014) sess706.pdf Thursday, March 20, 2014 [R706] POSTER SESSION: MARS CRYOSPHERE 6:00 p.m. Town Center Exhibit Area Guidat T. Pochat S. Bourgeois O. Soucek O. POSTER LOCATION #101 Early Hesperian Warm-Based Glaciation in Isidis Planitia, Mars [#1800] We propose to interpret the origin of Isidis Planitia landforms based on a new geomorphic mapping initiative that elucidates their interrelationship. Fassett C. I. Levy J. S. Head J. W. Dickson J. L. POSTER LOCATION #102 Long-Lived Glaciation in the Northern Mid-Latitudes of Mars: New Constraints on Timing [#1494] Landforms inferred to be the result of glaciation are common in the northern mid-latitudes of Mars. We focus here on the timing and persistence of glaciation. Scanlon K. E. Head J. W. POSTER LOCATION #103 The Dorsa Argentea Formation: Synthesis of Glacial Features and History of Late Noachian-Early Hesperian Martian Climate Change [#1477] We use the timing of ice advance and retreat recorded by glacial features in the DAF to synthesize a history of the ice sheet and early Mars climate change. Scanlon K. E. Head J. W. Marchant D. R. POSTER LOCATION #104 Evidence for Local, Volcanism-Induced Wet-Based Glacial Conditions in the Amazonian Arsia Mons Fan-Shaped Deposit [#1480] Several regions of the Arsia Mons Fan-Shaped Deposit show that volcano-ice interactions induced local wet-based behavior in the otherwise cold-based glacier. Hughes A. C. G. Hauber E. Rossi A. P. POSTER LOCATION #105 Geomorphology of Glacial and Periglacial Landforms Within a Small Crater in Terra Cimmeria, Mars: Stratigraphy and Inferred Chronology of Processes [#1211] We present a geomorphological map of a crater in Terra Cimmeria, Mars, and reconstruct the complex history of glacial and periglacial processes in this crater. Johnsson A. Reiss D. Hauber E. Hiesinger H. POSTER LOCATION #106 Possible Slow Periglacial Mass Wasting on Interior Crater Walls on Southern Mars [#1105] Small-scale lobate landforms that may be indicative of recent freeze-thaw activity are cataloged on the southern hemisphere on Mars. Jawin E. R. Head J. W. Marchant D. R. POSTER LOCATION #107 Paraglacial Geomorphology on Mars: Application to Post-Glacial Features in Martian Impact Craters [#2241] We apply paraglacial geomorpholgy to martian craters bearing evidence of glaciation to suggest young geologic features form in a post-glacial environment. Chuang F. C. Crown D. A. Berman D. C. POSTER LOCATION #108 Glacial Modification of Eastern Nereidum Montes, Mars: Observations from Southern Hemisphere Mapping of Lobate Debris Aprons and Ice-Rich Flow Features [#2066] Eastern Nereidum Montes is a region on Mars that appears to have experienced significant past glacial activity from THEMIS IR and CTX observations. Chuang F. C. Crown D. A. Berman D. C. Joseph E. C. S. POSTER LOCATION #109 Lobate Debris Aprons and Ice-Rich Flow Features in Eastern Hellas, Mars: Mapping Using THEMIS IR and CTX Data [#2081] The mapping of lobate debris aprons (LDAs) and other ice-rich flow features in eastern Hellas, Mars, was significantly improved using THEMIS IR and CTX data. 45th Lunar and Planetary Science Conference (2014) sess706.pdf Petersen E. I. Holt J. W. Berney J. E. POSTER LOCATION #110 A Comparative Study of Martian Lobate Debris Aprons to Assess Regional Differences in Surface Properties, Morphology, and Internal Composition [#2784] A comparative study of LDAs across the dichotomy boundary region of Deuteronilus Mensae using radar, morphology, and topography to constrain regional trends. Cardenas B. T. Lalich D. E. Petersen E. McKinnon E. A. Andry C. M. et al. POSTER LOCATION #111 Assessing the Potential of Debris-Covered Glaciers in the Uinta Mountains as Martian Analogs [#2362] GPR and LiDAR scans of debris-covered glaciers in the Uinta Mountains, Utah, will assess their potential as terrestrial analogs to martian lobate debris aprons. Berman D. C. Crown D. A. Chuang F. C. POSTER LOCATION #112 Preservation and Mobilization of Ice-Rich Mantling Deposits in Nereidum Montes, Mars [#1553] Nereidum Montes on the northern rim of Argyre Basin contains extensive preservation of ice-rich mantling deposits and associated features. Fastook J. L. Head J. W. POSTER LOCATION #113 Concentric Crater Fill: Rates of Glacial Accumulation, Infilling and Deglaciation in the Amazonian and Noachian of Mars [#1227] A coupled ice-flow/advected-debris model is used to assess two formation scenarios: (1) A single persistent mantling event, (2) multiple transient mantling events. Mattson S. Kilgallon A. Byrne S. McEwen A. S. Herkenhoff K. et al. POSTER LOCATION #114 Meter-Scale Pits in Mars’ North Polar Layered Deposits [#2431] We report the discovery in HiRISE images of meter-scale pits in the north polar layered deposits on Mars. Possible formation hypotheses are briefly discussed. Landis M. E. Byrne S. Daubar I. J. POSTER LOCATION #115 Reinterpreting the Impact Craters of the North Polar Layered Deposits, Mars [#2661] We use the Daubar et al. (2013) production function and updated HiRISE images to reinterpret the impact crater population of the north polar layered deposits. Lalich D. E. Holt J. W. POSTER LOCATION #116 Investigating Layer Properties of the Martian NPLD Using SHARAD Observations and Modeling [#2210] We use a simple plane wave propagation model to estimate the dielectric properties of the upper martian NPLD. Smith I. B. Holt J. W. POSTER LOCATION #117 Regional Variability in the Spiral Troughs of the North Polar Layered Deposits, Mars, as Observed by SHARAD [#1392] We conducted a cap wide study of NPLD spiral troughs with SHARAD. Regional diversity is discussed based on morphological and stratigraphic features. Becerra P. Byrne S. Mattson S. Herkenhoff K. E. HiRISE Team POSTER LOCATION #118 Martian Polar Stratigraphy from HiRISE Stereo Topography [#2408] We present a new method to analyze the stratigraphy of the polar layered deposits based on high-resolution Digital Terrain Models (DTM) and wavelet analysis. Milkovich S. M. POSTER LOCATION #119 Surface Expression of Radar Reflections Within Promethei Lingula, South Polar Layered Deposits, Mars [#2098] Intersection of / Layers and reflections lead / To polar insights. 45th Lunar and Planetary Science Conference (2014) sess706.pdf Kreslavsky M. A. Head J. W. POSTER LOCATION #120 Active Layer on Mars: When and Where? [#2715] Active layer sorting cannot explain rock circles in Elysium Planitia. Soliflucion lobes in several high N craters can result from a recent active layer episode. Hansen C. J. Diniega S. Bridges N. Byrne S. Dundas C. et al. POSTER LOCATION #121 Wind and Dry Ice: Agents of Change on Mars’ North Polar Erg [#1667] Both wind and seasonal CO2 ice sculpt the dunes in Mars’ north polar erg in today’s climate. Portyankina G. Hansen C. J. Aye K.-M. POSTER LOCATION #122 Differences in Seasonal CO2 Cover of Dune Slopes in Martian Northern Polar Erg [#2289] We are investigating the connection between extensive spring activity in martian polar erg and the modification of the dunes observed by HiRISE. Tyson S. Lane S. J. Wilson L. Gilbert J. S. POSTER LOCATION #123 Magma-Cryosphere Interactions on Mars — An Experimental Investigation of Physical Processes [#1124] We describe laboratory experiments on how simulated martian cryosphere reacts to heating by a sill-like intrusion causing ice melting and water/steam formation. Cassanelli J. P. Head J. W. Fastook J. L. POSTER LOCATION #124 Late Noachian “Icy Highlands” Mars: Implications for Melting and Ground-Water Recharge Across the Tharsis Rise [#1501] We investigate Late Noachian ice deposits across the Tharsis rise and the implications for melting in response to regionally elevated geothermal heat fluxes. Litvak M. L. Mitrofanov I. G. Boynton W. V. Fedosov F. Golovin D. et al. POSTER LOCATION #125 Following Subsurface Water Distribution in Past, Current and Future Mars Orbital and Surface Missions Based on the Neutron Spectroscopy Observations [#1842] The comparison of orbital and surface studies of subsurface water distribution at equatorial latitudes of Mars based on neutron spectrometry measurements. Bapst J. Bandfield J. L. Wood S. E. POSTER LOCATION #126 Investigating the Timing and Extent of Seasonal Surface Water Frost on Mars with MGS TES [#1594] We investigate the timing and extent of seasonal water frost on Mars’ surface using spaceborne instruments and lander observations. Piqueux S. Kleinböhl A. Hayne P. McCleese D. Kass D. et al. POSTER LOCATION #127 Climatological Growth and Recession Cycles of the Martian Seasonal Caps Using Thermal Emission Spectrometer (TES) and Mars Climate Sounder (MCS) Data [#1975] We present climatological (i.e., median) seasonal CO2 cap edge maps derived from eight Mars Years (MY) of surface observations by TES and MCS during clear years. Pilorget C. Edwards C. S. Ehlmann B. L. Forget F. Millour E. POSTER LOCATION #128 Material Ejection by the Colds Jets and Temperature Evolution of the South Seasonal Polar Cap of Mars from THEMIS/CRISM Observations and Implications for the Surface Properties [#1538] We have used CRISM and THEMIS data along with a thermal numerical model to quantify the amount of material ejected by the cold jets on the Mars polar caps. Travis B. J. Feldman W. C. POSTER LOCATION #129 Factors Controlling Polygon Sizes in the Martian Near-Surface [#2568] Numerical hydrothermochemical flow simulations indicate that soil permeability and salt content are major determinants of martian polygon features. .
Load more

Recommended publications
  • Geomorphological Evidence of Local Presence of Ice-Rich Deposits in Terra Cimmeria, Mars
    Mars Workshop on Amazonian Climate 2018 (LPI Contrib. No. 2086) 4010.pdf Geomorphological Evidence of Local Presence of Ice-Rich Deposits in Terra Cimmeria, Mars. S. Adeli1, E. Hauber1, G. Michael2, P. Fawdon3, I. B. Smith4, and R. Jaumann1,2. 1Deutsches Zentrum fuer Luft- und Raum- fahrt (DLR), Institute für Planetenforschung, Rutherfordstr. 2, 12489 Berlin, Germany ([email protected]). 2Freie Universität Berlin, Institute of Geological Sciences, Malteserstr. 74-100, 12249 Berlin, Germany. 3Birkbeck, University of London, Malet St, London WC1E 7HX. 4Planetary Science Institute, 1546 Cole Blvd Ste 120, Lake- wood, Colorado, USA. Introduction: Global circulation models suggest a) that obliquity oscillations caused the mobilization of ice from polar regions and its re-deposition at lower latitudes [1, 2]. They show that during high obliquity periods, ice can be deposited almost anywhere in the mid-latitudes and during low obliquity ice is transport- ed back to the poles [2-4]. Although the obliquity vari- Tarq b ations are not predictable for periods more than 20 Ma Crater ago [6], it is likely that the surface of Mars, during Amazonian, has repeatedly undergone such climate changes leading to deposition and sublima- tion/evaporation of ice-rich material [e.g., 3, 6, 7]. Evidence of shallow ground ice has been widely ob- served in the north and south mid-latitude regions of Mars such as: geomorphological evidence of debris- covered glaciers [e.g., 8, 9] and SHARAD observation [e.g., 10] of ~70 m thick ice deposits. This study de- scribes well-preserved glacial-like deposits in Terra Cimmeria, which are defined here as valley fill depos- b) c) its (VFD) (Fig.
    [Show full text]
  • Geological Map of Terra Cimmeria, Mars
    51st Lunar and Planetary Science Conference (2020) 2766.pdf GEOLOGIC MAP OF TERRA CIMMERIA, MARS. A. G. Siwabessy1,2, C. M. Rodrigue1, and R. C. Ander- son2, 1Department of Geography, California State University-Long Beach, 1250 Bellflower Boulevard, Long Beach, California 90840 ([email protected]), 2Geophysics and Planetary Geosciences Group, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Boulevard, Pasadena, CA 91109 Introduction: The Tharsis Rise dominates the ping area, trending into Hesperia Planum. Further to tectonic geomorphology of the western hemisphere of the northwest, a third type of basin – by far the least Mars. Anderson et al. [1] challenged the premise of mature of the three observed types – is observed. They [2], a prior study that presupposed that Tharsis uplift- are sometimes clearly associated with antecedent im- ed in a single event centered near Pavonis Mons. [1] pact structures. As they are occasionally connected by found instead that compressional and extensional fea- cascading sequences of downslope-incising valleys, tures across the western hemisphere are controlled by fluvial erosion may have occurred coevally with the five primary tectonic centers, of which the most an- regional uplift at [6]'s Hadriarca-Tyrrhena center. cient lies near the Claritas Rise. More recently, [3,4] Other than globally-distributed wrinkle ridge sets [8], studied putative basin and range topography on the explicit tectonic signatures associating Terra Cimme- southwest margin of the Tharsis Rise. [4] correlated ria to regional forcers (such as Tharsis) are not ob- the orientation of these features to predicted extension served. However, this does not necessarily limit forc- modeled by [5], but only if their model is rotated by ing effects of far-field activity – particularly from 12o and then re-centered not on the predicted regime Tharsis – from controlling the basin’s subsurface ge- by [2] but on the Stage 1 Claritas center of [1].
    [Show full text]
  • 20040191780.Pdf
    Second Conference on Early Mars (2004) 8013.pdf EROSIONAL HISTORY OF THE MARTIAN HIGHLANDS DURING THE NOACHIAN AND HESPERIAN. A. D. Howard1, J. M. Moore2, R. A. Craddock 3, and R. P. Irwin, III3, 1Department of Environmental Sciences, P.O. Box 400123, University of Virginia, Charlottesville, VA 22904-4123, [email protected]. 2NASA Ames Research Center, MS 245-3, Moffett Field, CA, 94035-100, 3Center for Earth and Planetary Studies, NASA Air and Space Museum, Washington, D.C. 20560. Introduction: The environment and erosional [12]). The statistics of degraded crater infilling and history of Mars early in its history has been a subject crater counts in the highlands are consistent with of debate since the first global imaging from Mariner degradation primarily by fluvial processes at a rate that 9. We present a synthesis that reflects our conclusion was proportional to the rate of new impacts [13], that fluvial erosion was widespread and intensive implying a gradual decline in fluvial activity. throughout the Noachian, extending into the Noachian environment. The environment that Hesperian. supported such intensive erosion during the Noachian Earliest Noachian: Frey and colleagues [1, 2] erosion is controversial [4], but the prevailing have identified numerous muted basins in the interpretation is that widespread, although episodic, highlands and lowlands constituting a population of precipitation (as snow or rain) occurred with associated highly degraded earliest Noachian impacts. They runoff and groundwater seepage. The abundance of interpret the basins to be buried by later deposits, with alluvial plains at the base of crater walls and the small much of the extant relief due to differential compaction number of breached crater rims suggests an arid [3].
    [Show full text]
  • Journal of Geophysical Research
    Journal Code Article ID Dispatch: 05.12.18 CE: MAS Revised proofs are sent only in the case of J G R E 21053No.ofPages: 21 ME: extensive corrections upon request 1 2 3 4 5 Journal of Geophysical Research: Planets 6 7 RESEARCH ARTICLE Evolution of Escarpments, Pediments, and Plains 8 9 10.1029/2018JE005681 in the Noachian Highlands of Mars 10 11 1 1 Key Points: Jon C. Cawley and Rossman P. Irwin III Q212 Q3 • Debris-mantled escarpments, Q5 13 regolith pediments, sloping 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA aggradational surfaces, and 14 depositional plains formed on 15 Martian cratered terrain 16 • Noachian arid-zone geomorphology Abstract Extensive Noachian-aged intercrater planation surfaces comprise much of the southern included aqueous weathering of highlands of Mars. We mapped aggradational and stable to degradational surfaces in three study areas 17 basalt to fines, low-intensity fluvial with diverse relief elements and ages: the high and rugged relief of Libya Montes, the well-preserved 18 erosion, and deposition in basins 19 intercrater plains of Noachis Terra, and the rolling relief with more drainage development in Terra Cimmeria. • These processes smoothed and 20 sealed Noachian ejecta blankets, Here we describe four major geomorphic features that formed in these regions: debris-mantled escarpments, 21 which required little geomorphic regolith pediments, sloping aggradational surfaces, and depositional plains. We interpret that with tectonic work to form stable pediments 22 stability and an arid paleoclimate, these features supported slow pedogenesis, sediment transport, and 23 diagenesis over hundreds of millions of years during heavy impact bombardment.
    [Show full text]
  • Geologic History of Water on Mars
    GEOLOGIC HISTORY OF WATER ON MARS: REGIONAL EVOLUTION OF AQUEOUS AND GLACIAL PROCESSES IN THE SOUTHERN HIGHLANDS, THROUGH TIME Dissertation zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften (Dr. rer. nat) vorgelegt als kumulative Arbeit am Fachbereich Geowissenschaften der Freien Universität Berlin von SOLMAZ ADELI Berlin, 2016 Erstgutachter: Prof. Dr. Ralf Jaumann Freie Universität Berlin Institut für Geologische Wissenschaften Arbeitsbereich Planetologie sowie Deutsches Zentrum für Luft- und Raumfahrt Institut für Planetenforschung, Abteilung Planetengeologie Zweitgutachter: Prof. Dr. Michael Schneider Freie Universität Berlin Institut für Geologische Wissenschaften Arbeitsbereich Hydrogeologie Tag der Disputation: 22 July 2016 i To my mother and my grandmother, the two strong women who inspired me the most, to follow my dreams, and to never give up. تقديم به مادر و مادر بزرگم به دو زن قوى كه الهام دهنده ى من بودند تا آرزو هايم را دنبال كنم و هرگز تسليم نشوم ii iii EIDESSTATTLICHE ERKLAERUNG Hiermit versichere ich, die vorliegende Arbeit selbstständig angefertigt und keine anderen als die angeführten Quellen und Hilfsmittel benutzt zu haben. Solmaz Adeli Berlin, 2016 iv v Acknowledgement First of all, I would like to thank my supervisor Prof. Dr. Ralf Jaumann for giving me the opportunity of working at the Deutsches Zentrum für Luft- und Raumfahrt (DLR). I wish to thank him particularly for standing behind me in all the ups and downs. Herr Jaumann, I am so deeply grateful for your support and your trust. Danke schön! This work would have not been achieved without the support of Ernst Hauber, my second supervisor. I have also been most fortunate to be able to work with him, and I have greatly appreciated the countless hours of discussions, all his advice regarding scientific issues, his feedbacks on my manuscripts, and everything.
    [Show full text]
  • MARS ORBITAL DATA — METHODS and INTERPRETATION 6:30 P.M
    Lunar and Planetary Science XXXIX (2008) sess614.pdf Thursday, March 13, 2008 POSTER SESSION II: MARS ORBITAL DATA — METHODS AND INTERPRETATION 6:30 p.m. Fitness Center Farrand W. H. Johnson J. R. Schmidt M. E. Bell J. F. III VNIR Spectral Differences on Natural and Brushed/Wind-abraded Surfaces on Home Plate, Gusev Crater, Mars: Spirit Pancam and HiRISE Color Observations [#1774] Color differences between the eastern and western rims of Home Plate are examined using Spirit Pancam and HiRISE color observations. Differences between near-field and remote observations are considered. Rice M. S. Bell J. F. III Wang A. Cloutis E. A. Vis-NIR Spectral Characterization of Si-rich Deposits at Gusev Crater, Mars [#2138] The Spirit rover has discovered high concentrations of silica at Gusev Crater, and a distinct spectral feature near 1000 nm appears to be diagnostic of these materials. We hypothesize that the presence of H2O or OH may be responsible for this feature. Combe J.-Ph. McCord T. B. Mars-Express/HRSC Spectral Data of MER Landing Sites Analyzed by a Multiple-Endmember Linear Spectral Linear Unmixing Model (MELSUM) [#2381] HRSC multispectral data are analyzed for mapping the main surface spectral components and photometric properties of Mars. The unique geometry of observation of this dataset is investigated. Results will be compared to field observations from the MERs. Hauber E. Gwinner K. Gendrin A. Fueten F. Stesky R. Pelkey S. Reiss D. Zegers T. E. MacKinnon P. Jaumann R. Bibring J.-P. Neukum G. Hebes Chasma, Mars: Slopes and Stratigraphy of Interior Layered Deposits [#2375] We present new data from HRSC and CTX on the topography, stratigraphy, and structure of Interior Layered Deposits in Hebes Chasma, Valles Marineris, Mars.
    [Show full text]
  • Compressional Tectonism on Mars
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 98, NO. E9, PAGES 17,049-17,060, SEPTEMBER 25, 1993 Compressional Tectonism on Mars THOMAS R. WATTERS Centerfor Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington,D.C. Contractional features on Mars were identified on the basis of photogeologic evidence of crustal shortening and comparison with terrestrial and planetary analogs. Three classes of structures, wrinkle ridges. lobate scarps and high-relief ridges. were mapped and their spatial and temporal distribution assessed. Wrinkle ridges account for over 80% of the total cumulative length of the mapped contractional features and occur in smooth plains material interpreted to be volcanic in origin. Lobate scarps, not wrinkle ridges, are the dominant contractional feature in Martian highland material. The pattern of contractional features in the western hemisphere reflects the hemispheric-scale iduence of the Tharsis rise. Although no comparable hemispheric- scale pattern is observed in the eastern hemisphere, prominent regional-scale patterns exist, the most notable of which occurs in Hesperia Planum. Contractional features that locally parallel the trend of the cmstal dichotomy boundary in the eastern hemisphere suggest the influence of stresses related to the evolution of the dichotomy. Compressional deformation apparently peaked during the Early Hesperia, if the tectonic features are roughly the same age as the units in which they occur. This peak in compressional deformation corresponds with Early Hesperian volcanic resurfacing of a large portion of the planet. Thermal history models for Mars, based on an initially hot planet, are inconsistent with estimates of the timing of peak compressional tectonism and the rate of volcanism.
    [Show full text]
  • Ross Irwin's CV
    Rossman Philip Irwin III Smithsonian Institution, National Air and Space Museum Center for Earth and Planetary Studies, MRC 315, Independence Ave. at 6th St. SW, Washington DC 20013 (p) 202.633.3632 (f) 202.633.4225 (e) [email protected] https://airandspace.si.edu/people/staff/ross-irwin EMPLOYMENT 2012–pres. & Smithsonian Institution, National Air and Space Museum, Washington, DC 2001-2010 CEPS Chair: 2019–pres. Geologist: Research on Martian and terrestrial desert geomorphology and paleohydrology, 2012–pres. Geologist: Pre- and post-doctoral research, 2001–2010. 2010–2012 Planetary Science Institute, Tucson, AZ Research Scientist: Fluvial geomorphology of early Mars and Titan, planetary geologic mapping, landing site characterization, and field studies of Mars-analog landforms. Visiting Scientist: NASA Goddard Space Flight Center, Greenbelt, MD. 1999-2001 Science Applications International Corporation, McLean, VA GIS Analyst: Web design, technical editing, and GIS support for VMap1 Coproducer Working Group (National Imagery and Mapping Agency client). University of Virginia Department of Environmental Sciences, Charlottesville, VA 2001 Teaching Assistant: Orphaned Lands Assessment (abandoned mineral mines and quarries) 1997-1999 Teaching Assistant: GIS, Physical Geology, Rocks and Minerals, Structural Geology Labs 1998-1999 Research Assistant: Viking spacecraft image processing and photomosaics 1997-1998 Southern Environmental Law Center, Charlottesville, VA Intern: research on non-point source pollution, environmental effects of suburban
    [Show full text]
  • The Case for Rainfall on a Warm, Wet Early Mars Robert A
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. E11, 5111, doi:10.1029/2001JE001505, 2002 The case for rainfall on a warm, wet early Mars Robert A. Craddock Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, District of Columbia, USA Alan D. Howard Department of Environmental Sciences, University of Virginia, Charlottesville, Virginia, USA Received 11 April 2001; revised 10 April 2002; accepted 10 June 2002; published 23 November 2002. [1] Valley networks provide compelling evidence that past geologic processes on Mars were different than those seen today. The generally accepted paradigm is that these features formed from groundwater circulation, which may have been driven by differential heating induced by magmatic intrusions, impact melt, or a higher primordial heat flux. Although such mechanisms may not require climatic conditions any different than today’s, they fail to explain the large amount of recharge necessary for maintaining valley network systems, the spatial patterns of erosion, or how water became initially situated in the Martian regolith. In addition, there are no clear surface manifestations of any geothermal systems (e.g., mineral deposits or phreatic explosion craters). Finally, these models do not explain the style and amount of crater degradation. To the contrary, analyses of degraded crater morphometry indicate modification occurred from creep induced by rain splash combined with surface runoff and erosion; the former process appears to have continued late into Martian history. A critical analysis of the morphology and drainage density of valley networks based on Mars Global Surveyor data shows that these features are, in fact, entirely consistent with rainfall and surface runoff.
    [Show full text]
  • Desktop Exploration of Remote Terrain (DERT). L. E. Keely1, L. J. Edwards1, and M
    3rd Planetary Data Workshop 2017 (LPI Contrib. No. 1986) 7005.pdf Desktop Exploration of Remote Terrain (DERT). L. E. Keely1, L. J. Edwards1, and M. C. Malin2, 1NASA (Ames Research Center, Moffett Field, CA), 2Malin Space Science Systems (San Diego, CA). Introduction: A digital terrain model (DTM) is a digital elevation model draped with one or more co- referenced orthoimages. NASA missions have provid- ed numerous DTMs for locations on Earth, Mars, and the Moon. However, these data sets are large and com- plex and somewhat underutilized due to the lack of dedicated software tools and documentation. DERT provides a basic 3D viewer for exploring NASA DTMs on the desktop. Building upon a rich software history from NASA Ames, DERT utilizes a virtual world to visualize and navigate the DTM. Additionally, DERT provides sev- Candor Chasma, Mars (HiRISE) with shadows de- eral tools that aid in understanding the topography and termined with JPL’s SPICE library. spatial relationships of terrain features. Data in both PDS and GeoTIFF formats are sup- ported. Files are preprocessed into multi-resolution image pyramids to improve rendering performance. DERT is open source and available at https://github.com/nasa/DERT. Pre-built releases for OS X and Linux are provided on the website. Terra Cimmeria, Mars (HiRISE) with CRISM chloride deposit layer Apollo 15 Landing Site (LROC) Arabia Terra, Mars (HiRISE) with cutting plane and difference map. Acknowledgements: Support for this work, part of the Mars Reconnaissance Orbiter Project, was provid- ed by NASA. Data are provided by NASA, JPL, Uni- Upheaval Dome, Utah (USGS) with terrain profile versity of Arizona, GFSC, ASU, and USGS.
    [Show full text]
  • Remanent Magnetization Signatures in Terra Cimmeria and Terra Sirenum
    51st Lunar and Planetary Science Conference (2020) 1996.pdf REMANENT MAGNETIZATION SIGNATURES IN TERRA CIMMERIA AND TERRA SIRENUM, MARS, AS A RESULT OF FAR-FIELD TECTONIC AND HYDROLOGICAL EFFECTS OF THE EARLY UPLIFT OF THE THARSIS RISE. A. G. Siwabessy1,2, C. M. Rodrigue1, and R. C. Anderson2, 1Department of Geography, California State University-Long Beach, 1250 Bellflower Boulevard, Long Beach, California 90840 ([email protected]), 2Geophysics and Planetary Geosciences Group, Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Boulevard, Pasadena, CA 91109 The Illinois, Michigan, and Williston basins consti- al. [17] additionally appears to correlate with the gen- tute possibly viable terrestrial analogues for under- eral form of the Eridania basin [18] (see Figure 2), standing the tectonic and hydrogeological context of potentially demarcating the spatial extent of magneti- the Eridania Basin in Terra Cimmeria and Terra Sire- zation associated with far-ranging metasomatic effects num, Mars. Although diagnostic tectonic geomorphol- of this proposed aquifer outflow from the Tharsis Ba- ogies are often not well-expressed at the surface in sin [after 4,5] in addition to valley networks sourced intracratonic basins themselves [1], orogenesis along by this groundwater [19]. The precipitation of single- the eastern plate margin of the North American craton phase magnetites into carbonates has been observed in has been successively tied both to coeval stratigraphic the meteorite ALH84001 and has been hypothesized to changes within each basin [2] and to the forcing of form a considerable fraction of subsurface stratigraphy metamorphic fluids from compressed aquifers perpen- in this region as a result of subsurface fluid fluxes, dicularly towards régimes of lower topography [3,4,5].
    [Show full text]
  • The Very Early Thermal State of Terra Cimmeria: Implications for Magnetic Carriers in the Crust of Mars Javier Ruiz
    The very early thermal state of Terra Cimmeria: Implications for magnetic carriers in the crust of Mars Javier Ruiz Cenno de Blologio MoleCulnr CSiC UnrverrldodAutonorna deMadnd 28049 Contoblonco, Modnd, Spoln ABSTRACT Large areas of shongly magnetized crust are located inTerra Cimmeria and Terra Sirenum, in the south ern hiehlands of Mars. the older terrains on the rilanet The tvuical deuth to the base of the maenetized crustal -eeotherms consistent with a orevious estimation oí the effective elastic thickness of the Iitho sphere, and with crustal abundanres of heat-producing elements based on swfare measurements per- formed by the Mars Odyssey Gamma Ray Spectrometer. The results suggest that, at the time of formation of the maenetized terrains surface fwhich have a minimum aee of 4.1 Gai. Cune de~thsfor magnetite and hematite were shallowet and similar, respectively, than the typical depth to the bze of the magnetized layer. This implies that hematite is an important (if not dominant) contributor to the magnetization of the martian must. However, an early warm climate would enhance the chance of mag- netite to be a iignificant. even dominant, magnetization carrier in the lower portion of the magneticlayer. 1. lntroduction lowland and locally thckw crust From the magnetic spectmm of Mars, Voorhies et al (2002) deduced an average thickness of The largest and strongly magnetized terrains on Mars are lo- -50 km for the maenetic crust. A refined studv bv Voarhles cated in Terra Cimmeria and Terra Sirenum (e.&. Acuña et al.. (2008)favoreda typic& depth of 47.8 + 8.4 km for báse óf the mag- 1999; Connerney et al., 2001).
    [Show full text]