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
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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. -
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. -
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). -
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. -
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). -
The Castalia Mission to Main Belt Comet 133P/Elst-Pizarro C
The Castalia mission to Main Belt Comet 133P/Elst-Pizarro C. Snodgrass, G.H. Jones, H. Boehnhardt, A. Gibbings, M. Homeister, N. Andre, P. Beck, M.S. Bentley, I. Bertini, N. Bowles, et al. To cite this version: C. Snodgrass, G.H. Jones, H. Boehnhardt, A. Gibbings, M. Homeister, et al.. The Castalia mission to Main Belt Comet 133P/Elst-Pizarro. Advances in Space Research, Elsevier, 2018, 62 (8), pp.1947- 1976. 10.1016/j.asr.2017.09.011. hal-02350051 HAL Id: hal-02350051 https://hal.archives-ouvertes.fr/hal-02350051 Submitted on 28 Aug 2020 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. Distributed under a Creative Commons Attribution| 4.0 International License 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. Snodgrass a,⇑, G.H. Jones b, H. Boehnhardt c, A. Gibbings d, M. Homeister d, N. Andre e, P. Beck f, M.S. Bentley g, I. Bertini h, N. Bowles i, M.T. Capria j, C. Carr k, M. -
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. -
Candidate Cave Entrances on Mars
G.E. Cushing – Candidate cave entrances on Mars. Journal of Cave and Karst Studies, v. 74, no. 1, p. 33–47. DOI: 10.4311/ 2010EX0167R CANDIDATE CAVE ENTRANCES ON MARS GLEN E. CUSHING U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA, [email protected] Abstract: This paper presents newly discovered candidate cave entrances into Martian near-surface lava tubes, volcano-tectonic fracture systems, and pit craters and describes their characteristics and exploration possibilities. These candidates are all collapse features that occur either intermittently along laterally continuous trench-like depressions or in the floors of sheer-walled atypical pit craters. As viewed from orbit, locations of most candidates are visibly consistent with known terrestrial features such as tube-fed lava flows, volcano-tectonic fractures, and pit craters, each of which forms by mechanisms that can produce caves. Although we cannot determine subsurface extents of the Martian features discussed here, some may continue unimpeded for many kilometers if terrestrial examples are indeed analogous. The features presented here were identified in images acquired by the Mars Odyssey’s Thermal Emission Imaging System visible- wavelength camera, and by the Mars Reconnaissance Orbiter’s Context Camera. Select candidates have since been targeted by the High-Resolution Imaging Science Experi- ment. Martian caves are promising potential sites for future human habitation and astrobiology investigations; understanding their characteristics is critical for long-term mission planning and for developing the necessary exploration technologies. INTRODUCTION cosmic rays (e.g., Mazur et al., 1978; De Angeles et al., 2002; Boston et al., 2004; Cushing et al., 2007). -
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). -
Orientation, Relative Age, and Extent of the Tharsis Plateau Ridge System
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 91. NO. 88. PAGES 8113-8125. JULY 10. 1986 Orientation, Relative Age, and Extent of the Tharsis Plateau Ridge System THOMAS R. WATTERS AND TED A. MAXWELL Center for Earth and Planetary Studies. National Air and Space Museum. Smithsonian Institution, Washington, D. C. The Tharsis ridge system is roughly circumferential to the regional topographic high of northern Syria Planum and the major Tharsis volcanoes. However, many of the ridges have orientations that deviate from the regional trends. Normals to vector means of ridge orientations, calculated in 10° boxes of latitude and longitude, show that the Tharsis ridges are not purely circumferential. Intersections of vector mean orientations plotted as great circles on a slereographic net show that the ridges are not concentric to a single point but to three broad zones. These data indicate either that the Tharsis ridge system did not form in response to a single regional compressional event with a single stress center or that the majority of the ridge system did form in a single event but with locally controlled deflections in the generally radially oriented stress field. Superposition relationships and relative ages suggest that the compressional stresses that produced the ridges occurred after the emplacement of the ridged plains volcanic units (early in the Hesperian period) but did not extend beyond the time of emplacement of the Syria Planum Formation units or the basal units of the Tharsis Montes Formation (during the latter half of the Hesperian period). Comparison of topographic data with the locations of ridges demonstrates a good correlation between the topographic edge of the Tharsis rise and outer extent of ridge occurrence. -
Preliminary Volcanic Feature Analysis of Olympus and Ascraeus Mons, Mars
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2407.pdf Preliminary Volcanic Feature Analysis of Olympus and Ascraeus Mons, Mars. K.J. Mohr1, D.A. Williams1, W.B. Garry2, and Jacob E. Bleacher2 1School of Earth & Space Exploration, Arizona State University, Tempe, AZ 85282, [email protected], 2Planetary Geology, Geophysics, and Geochemistry Laboratory, Code 698, NASA Goddard Space Flight Center, Greenbelt, MD 20771. Introduction/Background: Olympus Mons (OM) Only features observed on the flanks of the and Ascraeus Mons (AM) are two large shield volcanoes were used in this study. However, future volcanoes found in the Tharsis province on Mars. Both work will include small shields found on the volcanoes have been recently mapped at a 1:1,000,000 surrounding plains of each of the Tharsis Montes. scale using high resolution imagery [1,2]. Mapping of Geologic Observations: Both Olympus Mons and Arsia and Pavonis Montes are still in progress. With the Ascraeus Mons are dominated by flank channel flows completion of the Olympus and Ascraeus Montes maps, that embay older flank ridge flows, suggesting a change direct comparison of volcanic features found on each in lava properties from a less viscous effusive flow to a edifice can be done. Rose diagram analysis shows more viscous effusive flow [1,2]. Lava fans are also strong similarities in specific features found on the two observed on both volcanoes, which are fan-like features large volcanoes, further suggesting a similar formation where a sudden change in slope allowed for a tube-fed and evolution. flow or vent to extrude lava into a deltaic shape. -
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.