Volcanism on Mars
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Planetary Geologic Mappers Annual Meeting
Program Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 Planetary Geologic Mappers Annual Meeting June 12–14, 2018 • Knoxville, Tennessee Institutional Support Lunar and Planetary Institute Universities Space Research Association Convener Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Science Organizing Committee David Williams, Chair Arizona State University Devon Burr Earth and Planetary Sciences Department, University of Tennessee Knoxville Robert Jacobsen Earth and Planetary Sciences Department, University of Tennessee Knoxville Bradley Thomson Earth and Planetary Sciences Department, University of Tennessee Knoxville Abstracts for this meeting are available via the meeting website at https://www.hou.usra.edu/meetings/pgm2018/ Abstracts can be cited as Author A. B. and Author C. D. (2018) Title of abstract. In Planetary Geologic Mappers Annual Meeting, Abstract #XXXX. LPI Contribution No. 2066, Lunar and Planetary Institute, Houston. Guide to Sessions Tuesday, June 12, 2018 9:00 a.m. Strong Hall Meeting Room Introduction and Mercury and Venus Maps 1:00 p.m. Strong Hall Meeting Room Mars Maps 5:30 p.m. Strong Hall Poster Area Poster Session: 2018 Planetary Geologic Mappers Meeting Wednesday, June 13, 2018 8:30 a.m. Strong Hall Meeting Room GIS and Planetary Mapping Techniques and Lunar Maps 1:15 p.m. Strong Hall Meeting Room Asteroid, Dwarf Planet, and Outer Planet Satellite Maps Thursday, June 14, 2018 8:30 a.m. Strong Hall Optional Field Trip to Appalachian Mountains Program Tuesday, June 12, 2018 INTRODUCTION AND MERCURY AND VENUS MAPS 9:00 a.m. Strong Hall Meeting Room Chairs: David Williams Devon Burr 9:00 a.m. -
What Is Hesperia Planum, Mars? an Examination of Multiple Working Hypotheses
Lunar and Planetary Science XXXVI (2005) 1962.pdf What is Hesperia Planum, Mars? An Examination of Multiple Working Hypotheses. Tracy K.P. Gregg1 and D.A. Crown2, 1Dept. of Geology, 876 Natural Sciences Complex, University at Buffalo, Buffalo, NY 14260, [email protected], 2David A. Crown, Planetary Science Institute, Tucson, AZ, [email protected]. Introduction: Hesperia Planum, Mars, ~1000 km to the southwest. Subsequent mapping characterized by a high concentration of mare-type and crater size-frequency distributions suggested an wrinkle ridges and ridge rings [1-4], encompasses a Amazonian age for this flow field [14]. Subsequent region of over 2 million square kilometers in the work [13-16] suggested that easily eroded volcanic southern highlands (Fig. 1). The most common deposits (interpreted to be pyroclastic deposits, interpretation is that the plains materials were probably flows) from Tyrrhena Patera extend several emplaced as“flood” lavas that filled in low-lying hundred kilometers to the northwest. Thus, only regions [5-10]. Deposit thickness, based on about one-third of what had originally been partially buried craters, is <3 km [4]. Its stratigraphic identified as Hesperia Planum ridged plains remains position and crater-retention age [e.g., 9, 11, 12; as such. In addition, Mest and Crown [17] map a Tanaka, 1986] define the base of the Hesperian dissected plains unit to the south of Tyrrhena Patera System. In addition, the mare-type wrinkle ridges on that may be a portion of Hesperia Planum modified its surface make Hesperia Planum the type locale for by fluvial activity, and Crown and Mest [18] note “Hesperian-aged ridged plains” on Mars [e.g., 9]. -
The Evolution of a Heterogeneous Martian Mantle: Clues from K, P, Ti, Cr, and Ni Variations in Gusev Basalts and Shergottite Meteorites
Earth and Planetary Science Letters 296 (2010) 67–77 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites Mariek E. Schmidt a,⁎, Timothy J. McCoy b a Dept. of Earth Sciences, Brock University, St. Catharines, ON, Canada L2S 3A1 b Dept. of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA article info abstract Article history: Martian basalts represent samples of the interior of the planet, and their composition reflects their source at Received 10 December 2009 the time of extraction as well as later igneous processes that affected them. To better understand the Received in revised form 16 April 2010 composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites Accepted 21 April 2010 and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from Available online 2 June 2010 K-poor (as low as 0.02 wt.% K2O) in the shergottites to K-rich (up to 1.2 wt.% K2O) in basalts from the Editor: R.W. Carlson Columbia Hills (CH) of Gusev Crater; the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K2O (0.16 wt.% to below detection limit). The compositional dataset for the Gusev basalts is Keywords: more limited than for the shergottites, but it includes the minor elements K, P, Ti, Cr, and Ni, whose behavior Mars igneous processes during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the shergottites residuum). -
Observations of Mass Wasting Events in the Cerberus Fossae, Mars
51st Lunar and Planetary Science Conference (2020) 2404.pdf OBSERVATIONS OF MASS WASTING EVENTS IN THE CERBERUS FOSSAE, MARS. C. M. Dundas1, I. J. Daubar, 1U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001 ([email protected]), 2Brown University. Introduction: The Cerberus Fossae are a set of ge- Rockfall tracks are observed at several locations. ologically-young, steep-sided fissures in the Elysium These include both simPle falls and large events break- region of Mars, which aPPear to have been the source of ing into many individual tracks (Fig. 2). floods of both water and lava [e.g., 1–4]. They have also been proposed as the site of recent seismically-triggered mass wasting [5–6]. The latter Possibility is of Particular interest because the fossae are in the same region as the InSight lander and may be tectonically active [7-8]. This abstract reports on observations of active mass move- ment in and near the Cerberus Fossae using before-and- after comparisons of images acquired by the High Res- olution Imaging Science Experiment (HiRISE) [9]. Observations: Thirty-six locations were analyzed, mostly covering the Cerberus Fossae but also including some nearby craters and massifs. SloPe activity of some form was observed at ten of these locations, although in some cases it is minor. The observed mass wasting near the fossae can be divided into three categories: slope streaks [cf. 10], sloPe lineae, and rockfalls. Slope lineae in the fossae were Previously described [11–12]. Recent observations confirm that some of the lineae in the Cer- berus Fossae grow incrementally (Fig. -
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]. -
Chemin X-Ray Diffraction of the Windjana Sample
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Mineralogy, provenance, and diagenesis of a potassic 10.1002/2015JE004932 basaltic sandstone on Mars: CheMin X-ray diffraction Special Section: of the Windjana sample (Kimberley area, Gale Crater) The Mars Science Laboratory Rover Mission (Curiosity) at The Allan H. Treiman1, David L. Bish2, David T. Vaniman3, Steve J. Chipera4, David F. Blake5, Kimberley, Gale Crater, Mars Doug W. Ming6, Richard V. Morris6, Thomas F. Bristow5, Shaunna M. Morrison7, Michael B. Baker8, Elizabeth B. Rampe6, Robert T. Downs7, Justin Filiberto9, Allen F. Glazner10, Ralf Gellert11, Key Points: Lucy M. Thompson12, Mariek E. Schmidt13, Laetitia Le Deit14, Roger C. Wiens15, Amy C. McAdam16, • First mineralogical analysis of Cherie N. Achilles2, Kenneth S. Edgett17, Jack D. Farmer18, Kim V. Fendrich7, John P. Grotzinger8, sandstone on Mars 19 20 8 21 12 • Windjana sandstone very rich in Sanjeev Gupta , John Michael Morookian , Megan E. Newcombe , Melissa S. Rice , John G. Spray , sanidine, implying a trachyte source Edward M. Stolper8, Dawn Y. Sumner22, Ashwin R. Vasavada20, and Albert S. Yen20 rock • The source of Gale Crater sediments is 1Lunar and Planetary Institute, Houston, Texas, USA, 2Department of Geological Sciences, Indiana University, Bloomington, Indiana, an incredibly diverse igneous terrane USA, 3Planetary Science Institute,Tucson,Arizona,USA,4Chesapeake Energy Corporation, Oklahoma City, Oklahoma, USA, 5NASA Ames Research Center, Moffett Field, California, USA, 6Astromaterials -
Chronology of Hesperia Planum, Mars: New Constraints Using Impact Craters As Stratigraphic Markers
45th Lunar and Planetary Science Conference (2014) 2793.pdf CHRONOLOGY OF HESPERIA PLANUM, MARS: NEW CONSTRAINTS USING IMPACT CRATERS AS STRATIGRAPHIC MARKERS. S. C. Mest1,2 and D. A. Crown1, 1Planetary Science Institute, Tucson, AZ ([email protected]); 2NASA Goddard Space Flight Center, Greenbelt, MD. Introduction: Impact craters represent temporally Images are imported into ArcGIS for each crater and stratigraphically distinct events in the geologic analyzed. The margins of the continuous ejecta blanket, record of a planetary surface. They can be used to crater rim, and crater floor deposits are mapped, and the constrain the local and regional geologic history by diameters of superposed craters are measured. ArcGIS combining relative and absolute age estimates for crater is being used to calculate unit areas and record crater materials with observations of cross-cutting diameters. Crater size-frequency distribution statistics relationships between impact craters and other geologic are compiled using the methodology described in [15- features. Model ages derived for impact crater materials 18]; all craters (D>50 m) on a given surface are counted in Hesperia Planum (HP) are providing important while avoiding obvious secondary craters and secondary temporal constraints on emplacement of the ridged rays, chains, or clusters. These data are plotted on plains material, ridge-forming events, and fluvial isochrons [16-18] to assess relative age (Martian time- modification of the plains. This abstract presents results stratigraphic age) and estimate absolute age. The obtained from analyses of several large impact craters in production function used to determine the isochrons the Hesperia Planum region. includes both primaries and a component of Geologic Setting: Hesperia Planum (> 2 million “background” secondaries (i.e., secondaries not km2 in area) is characterized by a high concentration of included in rays, chains or clusters) [16-18]. -
AST-2018-1847-Ver9-Hughes 4P 260..283
ASTROBIOLOGY Volume 19, Number 3, 2019 Mary Ann Liebert, Inc. DOI: 10.1089/ast.2018.1847 Basaltic Terrains in Idaho and Hawai‘i as Planetary Analogs for Mars Geology and Astrobiology Scott S. Hughes,1 Christopher W. Haberle,2 Shannon E. Kobs Nawotniak,1 Alexander Sehlke,3 W. Brent Garry,4 Richard C. Elphic,3 Samuel J. Payler,5 Adam H. Stevens,5 Charles S. Cockell,5 Allyson L. Brady,6 Jennifer L. Heldmann,3,7 and Darlene S.S. Lim3,8 Abstract Field research target regions within two basaltic geologic provinces are described as Earth analogs to Mars. Regions within the eastern Snake River Plain of Idaho and the Big Island of Hawai‘i, the United States, provinces that represent analogs of present-day and early Mars, respectively, were evaluated on the basis of geologic settings, rock lithology and geochemistry, rock alteration, and climate. Each of these factors provides rationale for the selection of specific targets for field research in five analog target regions: (1) Big Craters and (2) Highway lava flows at Craters of the Moon National Monument and Preserve, Idaho, and (3) Mauna Ulu low shield, (4) Kılauea Iki lava lake, and (5) Kılauea caldera in the Kılauea Volcano summit region and the East Rift Zone of Hawai‘i. Our evaluation of compositional and textural attributes, as well as the effects of syn- and posteruptive rock alteration, shows that basaltic terrains in Idaho and Hawai‘i provide a way to characterize the geology and major geologic substrates that host biological activity of relevance to Mars exploration. This work provides the foundation to better understand the scientific questions related to the habitability of basaltic terrains, the rationale behind selecting analog field targets, and their applicability as analogs to Mars. -
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, -
Geology of Alba Mons, Mars: Results from 1:1M-Scale Geologic Mapping
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 2160.pdf GEOLOGY OF ALBA MONS, MARS: RESULTS FROM 1:1M-SCALE GEOLOGIC MAPPING. David A. Crown1, Daniel C. Berman1, Stephen P. Scheidt1, and Ernst Hauber3, 1Planetary Science Institute, 1700 E. Ft. Lowell Rd., Suite 106, Tucson, Arizona 85719 ([email protected]); 2Institute of Planetary Research, German Aerospace Center, Berlin, Germany. Introduction: Imaging and topographic datasets distribution and local slope, and the occurrence of are being used to produce two 1:1M-scale geologic dendritic networks on the highest local slopes, suggest maps of Alba Mons in order to document the volcanic control by topography rather than variations in evolution and geologic history of the northernmost substrate properties. volcano in the Tharsis region. We utilize geologic 2) Alba Mons’ western flank is dominated by lava mapping of Alba Mons’ summit region (245-255°E, flows and lava tube systems [24-26]. Their distribution 32.5-47.5°N) and western flank (230-245°E, 37.5- is consistent with the broad shape of the volcano and 47.5°N) to characterize volcanic, tectonic, and local slopes (i.e., at 50 km scale), although some lava erosional processes and derive age constraints from flow paths have been deflected by local obstacles, cross-cutting relationships and crater size-frequency including pre-existing craters and volcanic flows. distributions. Although local relationships are complex, lava flows Mapping Methodology and Datasets: Geologic generally seem to post-date adjacent lava tube systems. mapping uses THEMIS, HRSC, CTX, and HiRISE 3) Individual lava flows are typically elongate with images supported by HRSC and MOLA topography. -
Abstract STUBBLEFIELD, RASHONDA KIAM. Extensional Tectonics at Alba Mons, Mars
Abstract STUBBLEFIELD, RASHONDA KIAM. Extensional Tectonics at Alba Mons, Mars: A Case Study for Local versus Regional Stress Fields. (Under the direction of Dr. Paul K. Byrne). Alba Mons is a large shield volcano on Mars, the development of which appears to be responsible for tectonic landforms oriented radially and circumferentially to the shield. These landforms include those interpreted as extensional structures, such as normal faults and systems of graben. These structures, however, may also be associated with broader, regional stress field emanating from the volcano-tectonic Tharsis Rise, to the south of Alba Mons and centered on the equator. In this study, I report on structural and statistical analyses for normal faults proximal to Alba Mons (in a region spanning 95–120° W and 14–50° N) and test for systematic changes in fault properties with distance from the volcano and from Tharsis. A total of 11,767 faults were mapped for this study, and these faults were all measured for strike, length, and distance from Alba Mons and Tharsis. Additional properties were qualitatively and quantitatively analyzed within a subset of 62 faults, and model ages were obtained for two areas with crater statistics. Distinguishing traits for each structure population include fault properties such as strike, vertical displacement (i.e., throw) distribution profiles, displacement–length (Dmax/L) scaling, and spatial (i.e., cross-cutting) relationships with adjacent faults with different strikes. The only statistically significant correlation in these analyses was between study fault strike with distance from Tharsis. The lack of trends in the data suggest that one or more geological processes is obscuring the expected similarities in properties for these fault systems, such as volcanic resurfacing, mechanical restriction, or fault linkage. -
Explosive Lava‐Water Interactions in Elysium Planitia, Mars: Geologic and Thermodynamic Constraints on the Formation of the Tartarus Colles Cone Groups Christopher W
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115, E09006, doi:10.1029/2009JE003546, 2010 Explosive lava‐water interactions in Elysium Planitia, Mars: Geologic and thermodynamic constraints on the formation of the Tartarus Colles cone groups Christopher W. Hamilton,1 Sarah A. Fagents,1 and Lionel Wilson2 Received 16 November 2009; revised 11 May 2010; accepted 3 June 2010; published 16 September 2010. [1] Volcanic rootless constructs (VRCs) are the products of explosive lava‐water interactions. VRCs are significant because they imply the presence of active lava and an underlying aqueous phase (e.g., groundwater or ice) at the time of their formation. Combined mapping of VRC locations, age‐dating of their host lava surfaces, and thermodynamic modeling of lava‐substrate interactions can therefore constrain where and when water has been present in volcanic regions. This information is valuable for identifying fossil hydrothermal systems and determining relationships between climate, near‐surface water abundance, and the potential development of habitable niches on Mars. We examined the western Tartarus Colles region (25–27°N, 170–171°E) in northeastern Elysium Planitia, Mars, and identified 167 VRC groups with a total area of ∼2000 km2. These VRCs preferentially occur where lava is ∼60 m thick. Crater size‐frequency relationships suggest the VRCs formed during the late to middle Amazonian. Modeling results suggest that at the time of VRC formation, near‐surface substrate was partially desiccated, but that the depth to the midlatitude ice table was ]42 m. This ground ice stability zone is consistent with climate models that predict intermediate obliquity (∼35°) between 75 and 250 Ma, with obliquity excursions descending to ∼25–32°.