DOCSLIB.ORG

Young Lava Flows on the Eastern Flank of Ascraeus Mons: Rheological

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Young Lava Flows on the Eastern Flank of Ascraeus Mons: Rheological JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 112, E05011, doi:10.1029/2006JE002717, 2007 Click Here for Full Article Young lava flows on the eastern flank of Ascraeus Mons: Rheological properties derived from High Resolution Stereo Camera (HRSC) images and Mars Orbiter Laser Altimeter (MOLA) data H. Hiesinger,1,2 J. W. Head III,1 and G. Neukum3 Received 21 March 2006; revised 6 September 2006; accepted 30 November 2006; published 23 May 2007. [1] We report on estimates of the rheological properties of late-stage lava flows on the eastern flank of Ascraeus Mons, Mars. From previous studies it is known that the dimensions of flows reflect rheological properties such as yield strength, effusion rates, and viscosity. Our estimates are based on new high-resolution images obtained by the High Resolution Stereo Camera (HRSC) on board the European Space Agency’s Mars Express spacecraft in combination with Mars Orbiter Laser Altimeter (MOLA) data. Compared to earlier studies, the high spatial resolution of the HRSC and MOLA data allowed us to map 25 late-stage lava flows and to measure their dimensions, as well as their morphological characteristics, in greater detail. Our estimates of the yield strengths for these flows range from 2.0 Â 102 Pa to 1.3 Â 105 Pa, with an average of 2.1 Â 104 Pa. These values are in good agreement with estimates for terrestrial basaltic lava flows and are comparable to previous estimates derived for a small number of lava flows on Ascraeus Mons. Our investigation indicates that the effusion rates for the studied Ascraeus Mons flows are on average 185 m3 sÀ1, ranging from 23 m3 sÀ1 to 404 m3 sÀ1. These results are higher than earlier findings that indicate effusion rates of 18–60 m3 sÀ1, with an average of 35 m3 sÀ1. However, our effusion rates are similar to terrestrial effusion rates of Kilauea and Mauna Loa and other Martian volcanoes. On the basis of our estimates of the effusion rates and the measured dimensions of the flows, we calculated that the time necessary to emplace the flows is on average 26 days. Viscosities were estimated on the basis of yield strengths and effusion rates, yielding average values of 4.1 Â 106 Pa-s and ranging from 1.8 Â 104 Pa-s to 4.2 Â 107 Pa-s. On the basis of newly available data sets (e.g., HRSC, MOLA) we are now able not only to identify possible differences in eruptive behavior between Ascraeus Mons and Elysium Mons but also to study such differences over time. Citation: Hiesinger, H., J. W. Head III, and G. Neukum (2007), Young lava flows on the eastern flank of Ascraeus Mons: Rheological properties derived from High Resolution Stereo Camera (HRSC) images and Mars Orbiter Laser Altimeter (MOLA) data, J. Geophys. Res., 112, E05011, doi:10.1029/2006JE002717. 1. Introduction Head, 1982; Banerdt et al., 1992; Breuer et al., 1996; 1.1. Geological Context Harder, 1998; Smith et al., 1999a, 1999b; Zuber et al., 2000; and references therein]. MOLA data indicate that the [2] The Tharsis Montes, Arsia Mons, Pavonis Mons, and Ascraeus Mons, are large volcanic constructs that are part of Tharsis bulge is topographically separated from Olympus the Tharsis bulge. The Tharsis bulge is commonly inter- Mons and Alba Patera and is located at the Martian preted to be the result of a long-lasting large mantle diapir dichotomy boundary [e.g., Smith et al., 1999a, 1999b; that due to the absence of plate tectonics on Mars, had Zuber et al., 2000]. The Tharsis Montes are the locations enough time to significantly uplift the lithosphere and of some of the youngest volcanic deposits on Mars [Scott initiate tectonic faulting and volcanism [e.g., Solomon and and Tanaka, 1986; Neukum et al., 2004a] and also show evidence for very recent glaciation [e.g., Head and Marchant, 2003; Head et al., 2003, 2005; Shean et al., 2004; Parsons 1Department of Geological Sciences, Brown University, Providence, and Head, 2004; Neukum et al., 2004a]. As discussed below, Rhode Island, USA. 2 the Tharsis Montes are considered to be large shield Institut fu¨r Planetologie, Westfa¨lische Wilhelms-Universita¨t, Mu¨nster, volcanoes [e.g., Pike, 1978; Scott and Tanaka, 1986; Germany. 3Institut fu¨r Geologische Wissenschaften, Freie Universita¨t Berlin, Greeley and Crown, 1990], but evidence has been presented Berlin, Germany. that indicates that these volcanoes might actually be com- posite volcanoes [Head and Wilson, 1998a, 1998b; Head Copyright 2007 by the American Geophysical Union. et al., 1998b]. 0148-0227/07/2006JE002717$09.00 E05011 1of24 E05011 HIESINGER ET AL.: RHEOLOGY OF ASCRAEUS MONS LAVA FLOWS E05011 Figure 1. Geologic map of the Tharsis Montes [Scott and Tanaka, 1986]. Ascraeus Mons is at the upper right of the map. 1.2. Dimensions of 0.26 b.y. for the central shield and 0.1–0.25 b.y. for the [3] Ascraeus Mons is the northern most (11°N, 256°E) caldera fill. More recent crater counts on the basis of HRSC of the Tharsis volcanoes (Figure 1) and has a base diameter data revealed very young model ages of 0.1 b.y. for the floor of 435 km and a caldera of about 55 km on average of the main caldera and up to 0.8 b.y. for the older smaller [Hodges and Moore, 1994]. On the basis of Mariner and calderas [Neukum et al., 2004a]. Finally, Schaber et al. Viking data, Hodges and Moore [1994] estimated the height [1978] counted craters on the surrounding plains immedi- of Ascraeus Mons to be on the order of 26 km, but MOLA ately northwest, west, and southwest of Ascraeus Mons. For data indicate that the summit of the volcano is about 18 km their unit K they found 300–500 craters larger than 1 km 6 2 high (Figure 2). per 10 km (N(1) = 300–500) and for their slightly older unit M they counted 850–1150 craters larger than 1 km per 1.3. Age 106 km2 (N(1) = 850–1150). Assuming that the Martian [4] Ascraeus Mons was previously mapped by Scott et al. crater production rate is a factor of two greater than that of [1981] as Hesperian to Amazonian in age (AHvu). Similar- the Moon, Schaber et al. [1978] calculated absolute ages of ly, in the geologic map of Scott and Tanaka [1986], 0.2–0.33 b.y. for unit K and 0.58–0.78 b.y. for unit M. Ascraeus Mons is mapped as member 3 (AHt3)ofthe Figure 3 is a compilation of stratigraphic systems [e.g., Tharsis Montes Formation, which is Hesperian to Amazo- Neukum and Wise, 1976; Tanaka et al., 1992; Hartmann nian in age (N(2) = 320–440; N(5) = 50–75). Crumpler and Neukum, 2001], crater density ranges for N(2), N(5), and Aubele [1978] counted craters on two Viking images, and N(16) [Scott and Tanaka, 1986], and ages of Ascraeus located on the southeast flank (90A49) and the summit area Mons volcanic deposits found in the literature [e.g., Schaber (90A50). Compared to other Martian volcanoes such as et al., 1978; Neukum and Hiller, 1981; Scott and Tanaka, Arsia and Pavonis Mons, they found low cumulative crater 1986; Hodges and Moore, 1994; Neukum et al., 2004a]. On size distribution slopes, which they interpreted as evidence the basis of data shown in Figure 3, we conclude that the for recent obliteration of small craters by numerous lava shield itself formed at least 1to1.5 b.y. ago, and that flows. Crater counts of Neukum and Hiller [1981] suggest a units M and K are slightly younger and probably contem- model age of the central shield of Ascraeus Mons of poraneous with the covering of the caldera floors by lava 1.3 b.y. and a model age of the caldera fill of 0.4– flows. From this discussion we further conclude that the 1.0 b.y. On the basis of a model developed by Soderblom et investigated flows are not only stratigraphically young (i.e., al. [1974], Hodges and Moore [1994] published model ages 2of24 E05011 HIESINGER ET AL.: RHEOLOGY OF ASCRAEUS MONS LAVA FLOWS E05011 Figure 2. MOLA topography and MOLA shaded relief map with superposed location of HRSC orbit h0016, which was used for this analysis. superposed on older flows), but are also very young in terms flows, distinct shield-like caldera complexes, and the ap- of absolute model ages. parent distinctiveness from other edifices interpreted to represent pyroclastic eruptions [e.g., Pike, 1978; Scott and 1.4. Structure Tanaka, 1986; Greeley and Crown, 1990]. However, Head [5] Are the Tharsis Montes and Ascraeus Mons in par- and Wilson [1998a, 1998b] and Head et al. [1998b] ticular, shield volcanoes or composite volcanoes? Bates and concluded that there is a strong theoretical and observational Jackson [1984, p. 463] define a shield volcano as ‘‘a broad, basis for a reinterpretation of the Tharsis Montes as gently sloping volcanic cone of flat domical shape, usually composite volcanoes. Support for an interpretation of the several tens or hundreds of square miles in extent, built Tharsis Montes as stratovolcanoes includes observations of chiefly of overlapping and interfingering basaltic lava edifice mantling material, flank fragmental deposits, lobe- flows. Typical examples are the volcanoes Mauna Loa shaped features, smooth deposits, summit cinder cones and and Kilauea on the island of Hawaii.’’ A composite volcano constructs, near-summit pit craters, the andesitic nature of or stratovolcano is described as ‘‘a volcano that is con- some flows, similarities to other pyroclastic deposits, differ- structed of alternating layers of lava and pyroclastic depos- ences between flank vent and edifice eruptions, and the its, along with abundant dikes and sills.
Load more

Recommended publications
  • 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).
    [Show full text]
  • Review of the MEPAG Report on Mars Special Regions
    THE NATIONAL ACADEMIES PRESS This PDF is available at http://nap.edu/21816 SHARE Review of the MEPAG Report on Mars Special Regions DETAILS 80 pages | 8.5 x 11 | PAPERBACK ISBN 978-0-309-37904-5 | DOI 10.17226/21816 CONTRIBUTORS GET THIS BOOK Committee to Review the MEPAG Report on Mars Special Regions; Space Studies Board; Division on Engineering and Physical Sciences; National Academies of Sciences, Engineering, and Medicine; European Space Sciences Committee; FIND RELATED TITLES European Science Foundation Visit the National Academies Press at NAP.edu and login or register to get: – Access to free PDF downloads of thousands of scientific reports – 10% off the price of print titles – Email or social media notifications of new titles related to your interests – Special offers and discounts Distribution, posting, or copying of this PDF is strictly prohibited without written permission of the National Academies Press. (Request Permission) Unless otherwise indicated, all materials in this PDF are copyrighted by the National Academy of Sciences. Copyright © National Academy of Sciences. All rights reserved. Review of the MEPAG Report on Mars Special Regions Committee to Review the MEPAG Report on Mars Special Regions Space Studies Board Division on Engineering and Physical Sciences European Space Sciences Committee European Science Foundation Strasbourg, France Copyright National Academy of Sciences. All rights reserved. Review of the MEPAG Report on Mars Special Regions THE NATIONAL ACADEMIES PRESS 500 Fifth Street, NW Washington, DC 20001 This study is based on work supported by the Contract NNH11CD57B between the National Academy of Sciences and the National Aeronautics and Space Administration and work supported by the Contract RFP/IPL-PTM/PA/fg/306.2014 between the European Science Foundation and the European Space Agency.
    [Show full text]
  • Aqueous Minerals from Arsia Chasmata of Arsia Mons, Tharsis Region: Implications for Aqueous Alteration Processes on Mars
    45th Lunar and Planetary Science Conference (2014) 1826.pdf AQUEOUS MINERALS FROM ARSIA CHASMATA OF ARSIA MONS, THARSIS REGION: IMPLICATIONS FOR AQUEOUS ALTERATION PROCESSES ON MARS. N. Jain*, S. Bhattacharya, P. Chauhan, Space Applications Centre (ISRO), Ahmedabad, Gujarat, India ([email protected]/ Fax: +91-079- 26915825). Introduction: The Arsia Chasmata is a complex help of high resolution data such as MGS-MOC (Mars collapsed region located at the northeastern flank of Global Surveyor-Mars Orbiter Camera), Viking orbiter Arsia Mons (figure 1 A and B) within Tharsis region [3], fresh appearing lava flows [4], graben and glaciers of planet Mars and is the most important region for the on flanks of Arsia Mons [5], young lava flows [6] study of minerals like phyllosilicate and pyroxene. The small shields at floor of caldera [7]. reflectance data of MRO-CRISM (figure 1 C D) has Present study mainly focuses on the mineralogy of confirmed above mentioned minerals in the study area. Arsia Chasmata which interestingly contains The presence of these minerals at the Arsia Chasmata absorption features of aqueous altered minerals such as on Mars provides the evidence of its past watery serpentine (phyllosilicate). This mineral is also located environment and their processes of formation. In the in Nili Fossae region which is long, narrow depression present study the absorption features of serpentine present on Mars [8]. But in the present study (phyllosilicate) are obtained at 2.32 µm, 1.94 µm and occurrence of this mineral at high altitude region raise 2.51 µm. Previous studies on Mars show that the curiosity to know about their formation processes.
    [Show full text]
  • THE 1:1,000,000 GEOLOGIC MAP of ARSIA MONS, MARS. W. B. Garry1, D. A. Williams2, A. M. Dapremont3 and D. E. Shean4 1NASA Goddard
    Planetary Geologic Mappers Meeting 2018 (LPI Contrib. No. 2066) 7028.pdf THE 1:1,000,000 GEOLOGIC MAP OF ARSIA MONS, MARS. W. B. Garry1, D. A. Williams2, A. M. Dapremont3 and D. E. Shean4 1NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, [email protected], 2School of Earth and Space Exploration, Arizona State University, Tempe, AZ, 85287, 3Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA, 30331, 4College of Engineering, University of Washington, Seattle, WA, 98195. Introduction: Arsia Mons, centered at 8.26°S and (MGS) Mars Orbiter Laser Altimeter (MOLA) topogra- 239.1°E, is the southernmost edifice of the three Tharsis phy [15] that reveal morphologic details and spatial re- Montes volcanoes on Mars. Each volcano has a similar, lationships appropriate for our mapping purposes. overall shape and structure [1, 2], but there are distinct Mapping Methods: Mapping was completed in spatial distributions of morphologic features that hint ESRI’s ArcMap™ 10.2. Line work was drawn at map each volcano has a slightly different evolution history scales of ~1:100,000 to ~1:50,000 with vertex spacing [3]. To determine the differences between these three of 500 m and registered to the THEMIS daytime infra- Martian shield volcanoes, we present a series of individ- red base map. The final ArcMap project includes loca- ual geologic maps of Arsia (this map), Pavonis [4], and tion features (points), linear features (lines), geologic Ascraeus Mons [5] based on high-resolution data sets to contacts (lines), and geologic map (polygons). show their similarities and differences.
    [Show full text]
  • 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
    [Show full text]
  • Volcanism on Mars
    Author's personal copy Chapter 41 Volcanism on Mars James R. Zimbelman Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC, USA William Brent Garry and Jacob Elvin Bleacher Sciences and Exploration Directorate, Code 600, NASA Goddard Space Flight Center, Greenbelt, MD, USA David A. Crown Planetary Science Institute, Tucson, AZ, USA Chapter Outline 1. Introduction 717 7. Volcanic Plains 724 2. Background 718 8. Medusae Fossae Formation 725 3. Large Central Volcanoes 720 9. Compositional Constraints 726 4. Paterae and Tholi 721 10. Volcanic History of Mars 727 5. Hellas Highland Volcanoes 722 11. Future Studies 728 6. Small Constructs 723 Further Reading 728 GLOSSARY shield volcano A broad volcanic construct consisting of a multitude of individual lava flows. Flank slopes are typically w5, or less AMAZONIAN The youngest geologic time period on Mars identi- than half as steep as the flanks on a typical composite volcano. fied through geologic mapping of superposition relations and the SNC meteorites A group of igneous meteorites that originated on areal density of impact craters. Mars, as indicated by a relatively young age for most of these caldera An irregular collapse feature formed over the evacuated meteorites, but most importantly because gases trapped within magma chamber within a volcano, which includes the potential glassy parts of the meteorite are identical to the atmosphere of for a significant role for explosive volcanism. Mars. The abbreviation is derived from the names of the three central volcano Edifice created by the emplacement of volcanic meteorites that define major subdivisions identified within the materials from a centralized source vent rather than from along a group: S, Shergotty; N, Nakhla; C, Chassigny.
    [Show full text]
  • 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.
    [Show full text]
  • Properties, Origins, and Preservation of Ancient Olivine-Bearing Bedrock: Implications for Noachian Processes on Mars, A
    Fourth Conference on Early Mars 2017 (LPI Contrib. No. 2014) 3033.pdf PROPERTIES, ORIGINS, AND PRESERVATION OF ANCIENT OLIVINE-BEARING BEDROCK: IMPLICATIONS FOR NOACHIAN PROCESSES ON MARS, A. D. Rogers1, J. C. Cowart1, J. W. Head2, N. H. Warner3, A. Palumbo2, and M. P. Golombek4, 1Stony Brook University, Stony Brook, NY, USA ([email protected]), 2Brown University, Providence, RI, USA, 3SUNY Geneseo, Geneseo, NY USA, 4Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA Introduction and significance: Many intercrater cratered terrains [10]. Even where Hesperian volcanic plains and degraded impact craters in the Noachian high- plains are in direct contact with older bedrock, a striking lands contain flat-lying, relatively high thermal inertia difference in TI and regolith cover is observed, such that (TI) surfaces (“bedrock”) that commonly show modest Hesperian plains are more mantled than the older subja- enrichments in olivine and/or pyroxene compared to sur- cent bedrock units [10] (Fig. 2). A candidate explanation rounding materials (Fig. 1). These surfaces have maxi- for this is that the Noachian bedrock was rapidly buried mum TI values above 500 J m-2 K-1 s-1/2 in THEMIS im- and then recently exposed [10], however an alternative ages; some units exhibit TI values well above 900 J m-2 explanation is that the Noachian bedrock units are me- K-1 s-1/2. These physicochemically distinctive units occur chanically weak/fine-grained materials that break up into in dozens of isolated exposures ranging from ~2x102 to fine-grained materials [e.g. 11,12] that are more easily ~3x104 km2 in area and exhibit morphologies indicating moved by wind.
    [Show full text]
  • 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.
    [Show full text]
  • The Alkaline Volcanic Rocks of Craters of the Moon National Monument, Idaho and the Columbia Hills of Gusev Crater, Mars Details
    The alkaline volcanic rocks of Craters of the Moon National Monument, Idaho and the Columbia Hills of Gusev Crater, Mars Details Meeting 2016 Fall Meeting Section Planetary Sciences Session Terrestrial Analogs for Planetary Processes: Oceans, Volcanoes, Impacts, and Dunes I Identifier P31E-01 Authors Haberle, C W*, Mars Space Flight Facility, Arizona State University, Tempe, AZ, United States Hughes, S S, Idaho State University, Idaho Falls, ID, United States Kobs-Nawotniak, S E, Department of Geosciences, Idaho State University, Idaho Falls, ID, United States Christensen, P R, Arizona State University, Tempe, AZ, United States Index Sediment transport [4558] Terms Atmospheres [5405] Titan [6281] Venus [6295] Abstract Idaho's Eastern Snake River Plain (ESRP) is host to extensive expressions of basaltic volcanism dominated by non evolved olivine tholeiites (NEOT) with localized occurrences of evolved lavas. Craters of the Moon National Monument (COTM) is a polygenetic lava field comprised of more than 60 lava flows emplaced during 8 eruptive periods spanning the last 15 kyrs. The most recent eruptive period (period A; 2500-2000 yr B.P.) produced flows with total alkali vs. silica classifications spanning basalt to trachyte. Coeval with the emplacement of the COTM period A volcanic pile was the emplacement of the Wapi and Kings Bowl NEOT 70 km SSE of COTM along the Great Rift. Previous investigations have determined a genetic link between these two compositionally distinct volcanic centers where COTM compositions can be generated from NEOT melts through complex ascent paths and variable degrees of fractionation and assimilation of lower-middle crustal materials. The Mars Exploration Rover, Spirit, conducted a robotic investigation of Gusev crater from 2004-2010.
    [Show full text]
  • Pre-Mission Insights on the Interior of Mars Suzanne E
    Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 2019 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. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1).
    [Show full text]
  • Adirondack Recreational Trail Advocates (ARTA)
    Adirondack Recreational Trail Advocates (ARTA) Proposal for the Adirondack Rail Trail Photo: Lake Colby Causeway, Lee Keet, 2013 Submitted by the Board of Directors of ARTA Tupper Lake: Hope Frenette, Chris Keniston; Maureen Peroza Saranac Lake: Dick Beamish, Lee Keet, Joe Mercurio; Lake Clear: David Banks; Keene: Tony Goodwin; Lake Placid: Jim McCulley; Beaver River: Scott Thompson New York State Snowmobile Association: Jim Rolf WWW.TheARTA.org Adirondack Recreational Trail Advocates P.O. Box 1081 Saranac Lake, N.Y. 12983 Page 2 This presentation has been prepared by Adirondack Recreational Trail Advocates (ARTA), a not-for- profit 501(c)(3) corporation formed in 2011 and dedicated to creating a recreational trail on the largely abandoned and woefully underutilized rail corridor . © 2013, Adirondack Recreational Trail Advocates, Inc. Page 3 Contents Executive Summary ...................................................................................................................................... 6 Original UMP Criteria Favor the Rail Trail .................................................................................................. 7 Changing the Status of the Corridor ........................................................................................................... 10 Classification as a Travel Corridor ......................................................................................................... 10 Historic Status ........................................................................................................................................
    [Show full text]