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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. -
Cold-Based Glaciation of Pavonis Mons, Mars: Evidence for Moraine Deposition During Glacial Advance Reid A
Parsons et al. Progress in Earth and Planetary Science (2020) 7:13 Progress in Earth and https://doi.org/10.1186/s40645-020-0323-9 Planetary Science RESEARCH ARTICLE Open Access Cold-based glaciation of Pavonis Mons, Mars: evidence for moraine deposition during glacial advance Reid A. Parsons1,2* , Tomohiro Kanzaki3, Ryodo Hemmi1 and Hideaki Miyamoto3 Abstract The three large volcanoes in the Tharsis region of Mars: Arsia, Pavonis, and Ascraeus Montes all have fan-shaped deposits (FSDs) on their northern or western flanks consisting of a combination of parallel ridges, knobby/ hummocky terrain, and a smooth, viscous flow-like unit. The FSDs are hypothesized to have formed in the Amazonian during a period of high spin-axis obliquity which redistributed polar ice to the equatorial Tharsis region resulting in thick (> 2 km), flowing ice deposits. Based on previous ice flow simulations and crater surveys, the ridges are interpreted to be recessional drop moraines formed as debris on the ice sheet surface was transported to the ice margin—forming a long ridge sequence over an extended (∼100 Myr) period of ice sheet retreat. We test this hypothesis using a high-resolution, thermomechanical ice sheet model assuming a lower ice loss rate (~ 0.5 mm/year) than prior work based on new experimental results of ice sublimation below a protective debris layer. Our ice flow simulation results, when combined with topographic observations from a long sequence of ridges located interior of the Pavonis FSD, show that the ridged units were more likely deposited during one or more periods of glacial advance (instead of retreat) when repetitive pulses (approx. -
Water and Lava Both Seem Viable for the Formation of One of Mars' Densest and Largest Channel Networks
EPSC Abstracts Vol. 14, EPSC2020-19, 2020 https://doi.org/10.5194/epsc2020-19 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Water and lava both seem viable for the formation of one of Mars' densest and largest channel networks Hannes Bernhardt and David A. Williams Arizona State University, School of Earth and Space Exploration, Tempe, United States of America ([email protected]) The Axius Valles on the Malea Planum region’s (MPR) northern flank down into the Hellas basin are one of the most extensive and densest channel networks on Mars [1,2]. While previous studies tentatively interpreted the area as pyroclastic deposits dissected by sapped water/lahar flows [3-8] we considered their viability versus low-viscosity lava flows. Physiography The Axius Valles and adjacent channels to the west consist of ~22,550 km of mostly parallel sinuous valleys dissecting a plain (drainage density of 0.09 km-1) of gentle but relatively uniform northnortheast tilt, i.e., long-wavelength dip, at ~0.6 to 0.9° (~1 to 1.6%) towards the Hellas basin floor. The channels are up to ~20 km wide and ~100 m deep, although most are narrower and shallower than ~5 km and ~50 m, respectively. The majority of the valleys originates around the rim of Amphitrites Patera between elevations of ~1,200 and ~1,600 m. Smaller subsets originate at or below the rim of Peneus Patera between elevations of ~0 m and ~600 m, or are traceable further south into the wrinkle-ridged plains of the MPR. -
Identification of Altered Silicate Minerals on Arsia, Pavonis and Ascraeus Mons of Tharsis Volcanic Provinces of Mars
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1851.pdf IDENTIFICATION OF ALTERED SILICATE MINERALS ON ARSIA, PAVONIS AND ASCRAEUS MONS OF THARSIS VOLCANIC PROVINCES OF MARS. Raj R. Patel1 and Archana M. Nair2, Indian Insti- tute of Technology Guwahati 781039, India, 1([email protected]), 2([email protected]). Introduction: Arsia mons (Figure 1: A, C and F), FRT00006DB6. H) MRO-CRISM image from Ascrae- Pavonis mons (Figure 1: A, D and G) and Ascraeus us mons: FRT000123CD. mons (Figure 1: A, E and H) are large shield volcanos located in Tharsis Volcanic Provinces (Figure 1: A and Study Area: Tharsis volcanic provinces of Mars B) of planet Mars. In the present study, reflectance data represents a continent sized region of anomalously of MRO-CRISM (Figure 1: F, G and H) was used to elevated terrain which contains largest volcanoes in the map silicate mineral pyroxene in Arsia chasmata, a solar system. Three shield volcanoes aligned SW- NE steep sided depression located in the northeastern flank Arsia mons, Pavonis mons and Ascraeus mons collec- of Arsia mons and in caldera region of Pavonis and tively known as Tharsis montes. Viking Orbiter data Ascraeus mons. The presence of these minerals pro- suggests that Arsia mons, Pavonis mons and Ascraeus vides the evidence for origin and formation of the mons had similar evolutionary trends [2]. Various ge- Tharsis provinces. Absorption features obtained from omorphological units have been found in all mons such the analysis are at 1.24 µm, 1.45 µm, 1.65 µm and 2.39 as lava flow, grabens and shield of caldera, etc. -
Modeling the Development of Martian Sublimation Thermokarst Landforms
Icarus 262 (2015) 154–169 Contents lists available at ScienceDirect Icarus journal homepage: www.journals.elsevier.com/icarus Modeling the development of martian sublimation thermokarst landforms a, b b Colin M. Dundas ⇑, Shane Byrne , Alfred S. McEwen a Astrogeology Science Center, U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA article info abstract Article history: Sublimation-thermokarst landforms result from collapse of the surface when ice is lost from the subsur- Received 8 August 2014 face. On Mars, scalloped landforms with scales of decameters to kilometers are observed in the mid- Revised 17 June 2015 latitudes and considered likely thermokarst features. We describe a landscape evolution model that cou- Accepted 29 July 2015 ples diffusive mass movement and subsurface ice loss due to sublimation. Over periods of tens of thou- Available online 21 August 2015 sands of Mars years under conditions similar to the present, the model produces scallop-like features similar to those on the martian surface, starting from much smaller initial disturbances. The model also Keywords: indicates crater expansion when impacts occur in surfaces underlain by excess ice to some depth, with Mars, surface morphologies similar to observed landforms on the martian northern plains. In order to produce these Geological processes Mars, climate landforms by sublimation, substantial quantities of excess ice are required, at least comparable to the vertical extent of the landform, and such ice must remain in adjacent terrain to support the non- deflated surface. We suggest that martian thermokarst features are consistent with formation by subli- mation, without melting, and that significant thicknesses of very clean excess ice (up to many tens of meters, the depth of some scalloped depressions) are locally present in the martian mid-latitudes. -
The Tharsis Montes, Mars: Comparison of Volcanic and Modified Landforms
I)oceamngs of Lunar and Pkmetmy Sdence, VVdume 22, pp. 31 -44 Lunar and Planetary INtihlte, Houston, 1992 The Tharsis Montes, Mars: Comparison of Volcanic and Modified Landforms James R Zimbelrnan Center for Eurtb and Planetary Studies, National Air and Space Museum, Smitbsonian Washington DC 20560 Kenneth S. Edgett The three 'Iharsis Montes shield volcanos, Arsia Mons, Pavonis Mons, and Axraeus Mons, have broad similarities that have been recognized since the Mariner 9 reconnaissance in 1972. Upon closer examination the volcanos are seen to have significant differences that are due to individual volcanic histories. AU three volcanos exhibit the following characteristics gentle (<5O) fkmk slopes, entrants in the northwestern and southeastern flanks that were the source for lavas extending away from each shield, summit caldera(s), and enigmatic lobe-shaped features extending over the plains to the west of each volcano. Zhe three volcanos display different degrees of circumferential graben and trough development in the summit regions, complexity of preserved caldera collapse events, secondary summit-region volcanic consuuction, and erosion on the lower western flanks due to mass wasting and the processes that formed the large lobe-shaped features. AU three lobe-shaped features start at elevations of 10 to 11 Ian and terminate at 6 km. The complex morphology of the lobe deposits appear to involve some form of catastrophic mass movement followed by efhsive and perhaps pyroclastic volcanism. subsequent materials (Scott and Tanuka, 1981). AU the rnate- rials on and around the Tharsis Montes are mapped as Upper The Tharsii Montes consist of three large shield volcanos Hesperian to Upper AInaZonian in age (Scott and Tanuka, named (firom south to north) Arsia Mom, Pavonis Mom, and 1986). -
Visible-To-Near-Infrared Spectral Variability of Hydrated Sulfates and Candidate Mars Landing Sites
Western Washington University Western CEDAR WWU Graduate School Collection WWU Graduate and Undergraduate Scholarship Winter 2018 Visible-to-Near-Infrared Spectral Variability of Hydrated Sulfates and Candidate Mars Landing Sites: Implications for the Mastcam- Z Investigation on NASA’s Mars-2020 Rover Mission Darian Dixon Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/wwuet Part of the Geology Commons Recommended Citation Dixon, Darian, "Visible-to-Near-Infrared Spectral Variability of Hydrated Sulfates and Candidate Mars Landing Sites: Implications for the Mastcam-Z Investigation on NASA’s Mars-2020 Rover Mission" (2018). WWU Graduate School Collection. 638. https://cedar.wwu.edu/wwuet/638 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]. Visible-to-Near-Infrared Spectral Variability of Hydrated Sulfates and Candidate Mars Landing Sites: Implications for the Mastcam-Z Investigation on NASA’s Mars-2020 Rover Mission By Darian Dixon Accepted in Partial Completion of the Requirements for the Degree Master of Science Kathleen L. Kitto, Dean of the Graduate School ADVISORY COMMITTEE Chair, Dr. Melissa Rice Dr. Pete Stelling Dr. Michael Kraft 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. -
Role of Glaciers in Halting Syrtis Major Lava Flows to Preserve and Divert a Fluvial System
ROLE OF GLACIERS IN HALTING SYRTIS MAJOR LAVA FLOWS TO PRESERVE AND DIVERT A FLUVIAL SYSTEM A Thesis Submitted to the Graduate Faculty of the Louisiana State University and Agricultural and Mechanical College in partial fulfillment of the requirements for the degree of Master of Geology in The Department of Geology and Geophysics by Connor Michael Matherne B.S., Louisiana State University, 2017 December 2019 ACKNOWLEDGMENTS Special thanks to J.R. Skok and Jack Mustard for conceiving the initial ideas behind this project and to Suniti Karunatillake and J.R. Skok for their guidance. Additionally, thank you to my committee members Darrell Henry and Peter Doran for aid in understanding the complex volcanic and climate history for this location. This work has benefited from reviews and discussions with Tim Goudge, Steven Ruff, Jim Head, and Bethany Ehlmann. We thank Caleb Fassett for providing the CTX DEM processing of the outlet fan and Tim Goudge for providing the basin Depression CTX DEM. All data and observations used in this study are publically available from the NASA PDS. Derived products such as produced CTX DEMs can be attained through processing or contacting the primary author. Connor Matherne was supported by the Frank’s Chair funds, W.L. Calvert Memorial Scholarship, NASA-EPSCoR funded LASpace Graduate Student Research Assistantship grant, and Louisiana Board of Regents Research Award Program grant LEQSF-EPS(2017)-RAP-22 awarded to Karunatillake. J.R. Skok was supported with the MDAP award NNX14AR93G. Suniti Karunatillake’s work was supported by NASA- MDAP grant 80NSSC18K1375. ii TABLE OF CONTENTS Acknowledgments.............................................................................................................. -
The Geological History of Nili Patera, Mars 10.1002/2015JE004795 P
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE The geological history of Nili Patera, Mars 10.1002/2015JE004795 P. Fawdon1, J. R. Skok2, M. R. Balme1, C. L. Vye-Brown3, D. A. Rothery1, and C. J. Jordan4 Key Points: 1Department of Physical Sciences, The Open University, Walton Hall, Milton Keynes, UK, 2Department of Geology & • A new CTX-scale map details the 3 geological history of Nili Patera Geophysics, Louisiana State University, Baton Rouge, Louisiana, USA, British Geological Survey, Murchison House, 4 • Magmatism includes effusive basalts, Edinburgh, UK, British Geological Survey, Nottingham, UK magmatic intrusion, and ignimbrite(s) • Volcanism and water suggest habitable environments in highland patera caldera Abstract Nili Patera is a 50 km diameter caldera at the center of the Syrtis Major Planum volcanic province. The caldera is unique among Martian volcanic terrains in hosting: (i) evidence of both effusive and explosive Supporting Information: volcanism, (ii) hydrothermal silica, and (iii) compositional diversity from olivine-rich basalts to silica-enriched • Figures S1 and S2 units. We have produced a new geological map using three mosaicked 18 m/pixel Context Camera digital • Map S1 elevation models, supplemented by Compact Remote Imaging Spectrometer for Mars Hyperspectral data. Correspondence to: The map contextualizes these discoveries, formulating a stratigraphy in which Nili Patera formed by trapdoor P. Fawdon, collapse into a volcanotectonic depression. The distinctive bright floor of Nili Patera formed either as part of a [email protected] felsic pluton, exposed during caldera formation, or as remnants of welded ignimbrite(s) associated with caldera formation—both scenarios deriving from melting in the Noachian highland basement. -
Scalloped Terrains in the Peneus and Amphitrites Paterae Region of Mars As Observed by Hirise
Icarus 205 (2010) 259–268 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Scalloped terrains in the Peneus and Amphitrites Paterae region of Mars as observed by HiRISE A. Lefort *, P.S. Russell, N. Thomas Space Research and Planetary Sciences, Physikalisches Institut, Universität Bern, 3012 Bern, Switzerland article info abstract Article history: The Peneus and Amphitrites Paterae region of Mars displays large areas of smooth, geologically young Received 10 October 2008 terrains overlying a rougher and older topography. These terrains may be remnants of the mid-latitude Revised 15 May 2009 mantle deposit, which is thought to be composed of ice-rich material originating from airfall deposition Accepted 3 June 2009 during a high-obliquity period less than 5 Ma ago. Within these terrains, there are several types of poten- Available online 14 June 2009 tially periglacial features. In particular, there are networks of polygonal cracks and scalloped-shaped depressions, which are similar to features found in Utopia Planitia in the northern hemisphere. This area Keywords: also displays knobby terrain similar to the so-called ‘‘basketball terrains” of the mid and high martian lat- Mars, Surface itudes. We use recent high resolution images from the High Resolution Imaging Science Experiment (HiR- Geological processes Ices ISE) along with data from previous Mars missions to study the small-scale morphology of the scalloped terrains, and associated polygon network and knobby terrains. We compare these with the features observed in Utopia Planitia and attempt to determine their formation process. While the two sites share many general features, scallops in Peneus/Amphitrites Paterae lack the diverse polygon network (i.e. -
The Tharsis Montes, Mars
Proceedings ofLunar and Planetary Science, Volume 22, pp. 31-44 Lunar and Planetary Institute, Houston, 1992 31 The Tharsis Montes, Mars: Comparison of Volcanic and Modified Landforms 1992LPSC...22...31Z James R. Zimbelman Center for l!artb and Planetary StruHes, National Mr and Space Museum, Smithsonian Institution, Washington DC 20560 Kenneth s. Edgett Department of Geology, Ari%ona Stale University, Tempe AZ 85287-1404 The three 1barsis Montes shield volcanos, Arsia Mons, Pavonis Mons, and Ascraeus Mons, have broad similarities that have been recognized since the Mariner 9 reco~ce in 1972. Upon closer examination the volcanos are seen to have significant differences that are due to individual volcanic histories. All three volcanos exhibit the following characteristics: gentle ( <5°) flank slopes, entrants in the northwestern and southeastern flanks that were the source for lavas extending away from each shield, summit caldera( s ), and enigmatic lobe-shaped features extending over the plains to the west of each volcano. The three volcanos display different degrees of circumferential graben and trough development in the summit regions, complexity of preserved caldera collapse events, secondary summit-region volcanic construction, and erosion on the lower western flanks due to mass wasting and the processes that funned the large lobe-shaped features. All three lobe-shaped features start at elevations of 10 to 11 km and terminate at 6 km. The complex morphology of the lobe deposits appear to involve some fonn of catastrophic mass movement followed by effusive and perhaps pyroclastic volcanism. INTRODUCfiON subsequent materials (Scott and Tanaka, 1981). All the mate- rials on and around the Tharsis Montes are mapped as Upper The Tharsis Montes consist of three large shield volcanos Hesperian to Upper Amazonian in age ( Scott and Tanaka, named (from south to north) Arsia Mons, Pavonis Mons, and 1986). -
Terrestrial Analogs to the Calderas of the Tharsis Volcanoes on Mars
File: {CUP_REV}Chapman-0521832926/Revises/0521832926c03.3d Creator: / Date/Time: 17.10.2006/5:48pm Page: 71/94 3 Terrestrial analogs to the calderas of the Tharsis volcanoes on Mars Peter J. Mouginis-Mark, Andrew J. L. Harris and Scott K. Rowland Hawaii Institute of Geophysics and Planetology, University of Hawaii at Manoa. 3.1 Introduction The structure and morphology of Martian calderas have been well studied through analysis of the Viking Orbiter images (e.g., Mouginis-Mark, 1981; Wood, 1984; Mouginis-Mark and Robinson, 1992; Crumpler et al., 1996), and provide important information on the evolution and eruptive styles of the parent volcanoes. Using Viking data it has been possible, for numerous calderas, to define the sequence of collapse events, identify locations of intra-caldera activity, and recognize post-eruption deformation for several calderas. Inferences about the geometry and depth of the magma chamber and intrusions beneath the summit of the volcano can also be made from image data (Zuber and Mouginis-Mark, 1992; Scott and Wilson, 1999). In at least one case, Olympus Mons, analysis of compressional and extensional features indicates that, when active, the magma chamber was located within the edifice (i.e., at an elevation above the surrounding terrain). The summit areas of Olympus and Ascraeus Montes provide evidence of a dynamic history, with deep calderas showing signs of having been full at one time to the point that lava flows spilled over the caldera rim (Mouginis-Mark, 1981). Similarly, shallow calderas contain evidence that they were once deeper (e.g., the western caldera of Alba Patera; Crumpler et al., 1996).