Terrestrial Shield Volcanoes: Mars

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Mars: The Tharsis Region and Shield Volcanoes GLY 424/524 March 4, 2002 Shield Volcanoes: Terrestrial Martian Volcanic Provinces • Basaltic • Shallow flank slopes (<11°) – 7 - 11° proximally – 4° distally • Summit calderas or caldera complexes • Hot-spots beneath ocean crust – Hawaii, Galapagos – Hot-spots beneath continental crust rarely produce shield volcanoes Tharsis Volcanoes Shield Volcanoes: Mars • Huge – Each one ~100x the volume of Hawaii – Why? • Tharsis – Olympus, Arsia, Pavonis, Ascraeus • Elysium Mons 1 Tharsis: Source • Mantle plume • Huge & long-lived • Antipodal to large impact? Olympus Mons • 27 km above m.p.r. • Basal diameter = 600 km • Basal scarp ~3-6 km tall – Locally draped by flows – Unique – Origin unknown • Summit caldera – Nested – 66 x 83 km Olympus Calderas on Shield Volcanoes Mons • Typically nested Caldera – Multpile episodes of magma “withdrawl” • Flank eruptions • Inflation and drainback – Relative ages determined by cross-cutting relations – No general temporal/spatial trend • Magma chamber – About same size as caldera width – About same depth as caldera width 2 Olympus Mons Caldera Ascraeus Mons Caldera Olympus Mons Flows MOC wide-angle • Tens of thousands lava flows drape flanks High-res here • Channel-fed & tube-fed • 102 - 103 km long • Similar in morphology to basaltic lava flows on Hawaii Olympus Mons Flows Mauna Loa, Hawaii Landsat image: phh = black; aa = red 3 Olympus Mons Olympus Mons Aureole lava flows Olympus Mons Aureole • As long as 600 km • Characterized by – Ridges – Troughs – Fractures – Graben Olympus Mons Aureole Aureole Formation • Sub-glacial eruption (table mountain) • Outwash flood deposits • Subaqueous eruption (seamount) • Landslide/debris aprons – Most folks believe this last one, but the VO image MOC wide-angle image question is far from answered Fov ~120 km MOC Narrow angle 4 Pavonis Mons • “Middle” volcano • Simple caldera Arsia Mons Elysium Mons Elysium Mons • Avg. flank slopes ~10° – Steeper than typical shield – Evolved composition? – Role of volatiles? • Dissolved water • Groundwater, groundice • Smaller than Tharsis uplift • Large channels on flank 5 Elysium Mons Elysium Mons • See MOC releases here • www.msss.com/mars_images/moc/7_10_98 _elysium_rel/ • 9 km tall • 240 km across Ages • Tharsis & Elysium mostly Hesperian • Tharsis began forming in Noachian • VERY young lava flows have been found in Elysium region (<10 Ma old) • Elysium region still active? 6.

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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.
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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.
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The Tharsis Montes, Mars: Comparison of Volcanic and Modified Landforms
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The Castalia Mission to Main Belt Comet 133P/Elst-Pizarro
Open Research Online The Open University’s repository of research publications and other research outputs The </i>mission to Main Belt Comet 133P/Elst-Pizarro Journal Item How to cite: Snodgrass, C.; Jones, G.H.; Boehnhardt, H.; Gibbings, A.; Homeister, M.; Andre, N.; Beck, P.; Bentley, M.S.; Bertini, I.; Bowles, N.; Capria, M.T.; Carr, C.; Ceriotti, M.; Coates, A.J.; Della Corte, V.; Donaldson Hanna, K.L.; Fitzsimmons, A.; Gutiérrez, P.J.; Hainaut, O.R.; Herique, A.; Hilchenbach, M.; Hsieh, H.H.; Jehin, E.; Karatekin, O.; Kofman, W.; Lara, L.M.; Laudan, K.; Licandro, J.; Lowry, S.C.; Marzari, F.; Masters, A.; Meech, K.J.; Moreno, F.; Morse, A.; Orosei, R.; Pack, A.; Plettemeier, D.; Prialnik, D.; Rotundi, A.; Rubin, M.; Sánchez, J.P.; Sheridan, S.; Trieloﬀ, M. and Winterboer, A. (2018). The Castalia mission to Main Belt Comet 133P/Elst-Pizarro. Advances in Space Research, 62(8) pp. 1947–1976. For guidance on citations see FAQs. c 2017 COSPAR https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.1016/j.asr.2017.09.011 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Available online at www.sciencedirect.com ScienceDirect Advances in Space Research 62 (2018) 1947–1976 www.elsevier.com/locate/asr The Castalia mission to Main Belt Comet 133P/Elst-Pizarro C.
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Terrestrial Analogs to the Calderas of the Tharsis Volcanoes on Mars
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Orientation, Relative Age, and Extent of the Tharsis Plateau Ridge System
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Preliminary Volcanic Feature Analysis of Olympus and Ascraeus Mons, Mars
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15. Volcanic Activity on Mars
15. Volcanic Activity on Mars Martian volcanism, preserved at the surface, composition), (2) domes and composite cones, is extensive but not uniformly distributed (Fig. (3) highland paterae, and related (4) volcano- 15.1). It includes a diversity of volcanic land- tectonic features. Many plains units like Lu- forms such as central volcanoes, tholi, paterae, nae Planum and Hesperia Planum are thought small domes as well as vast volcanic plains. to be of volcanic origin, fed by clearly defined This diversity implies different eruption styles volcanoes or by huge fissure volcanism. Many and possible changes in the style of volcanism small volcanic cone fields in the northern plains with time as well as the interaction with the are interpreted as cinder cones (Wood, 1979), Martian cryosphere and atmosphere during the formed by lava and ice interaction (Allen, evolution of Mars. Many volcanic constructs 1979), or as the product of phreatic eruptions are associated with regional tectonic or local (Frey et al., 1979). deformational features. An overview of the temporal distribution of Two topographically dominating and mor- processes, including the volcanic activity as phologically distinct volcanic provinces on Mars well as the erosional processes manifested by are the Tharsis and Elysium regions. Both are large outflow channels ending in the northern situated close to the equator on the dichotomy lowlands and sculpting large units of the vol- boundary between the cratered (older) high- canic flood plains has been given by Neukum lands and the northern lowlands and are ap- and Hiller (1981). This will be discussed in proximately 120◦ apart. They are characterized this work together with new findings.
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Mars Upside Down 14 December 2017
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