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Stähler SC, Khan A, Banerdt WB, Lognonné P, Giardini D, Ceylan S, Drilleau M, Duran AC, Garcia RF, Huang Q, Kim D, Lekic V, Samuel H, Schimmel M, Schmerr N, Sollberger D, Stutzmann É, Xu Z, Antonangeli D, Charalambous C, Davis PM, Irving JCE, Kawamura T, Knapmeyer M, Maguire R, Marusiak AG, Panning MP, Perrin C, Plesa AC, Rivoldini A, Schmelzbach C, Zenhäusern G, Beucler É, Clinton J, Dahmen N, van Driel M, Gudkova T, Horleston A, Pike WT, Plasman M, Smrekar SE. Seismic detection of the martian core. Science 2021; 373:443-448. [PMID: 34437118 DOI: 10.1126/science.abi7730] [Citation(s) in RCA: 80] [Impact Index Per Article: 26.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/01/2021] [Accepted: 06/14/2021] [Indexed: 11/02/2022]
Abstract
Clues to a planet's geologic history are contained in its interior structure, particularly its core. We detected reflections of seismic waves from the core-mantle boundary of Mars using InSight seismic data and inverted these together with geodetic data to constrain the radius of the liquid metal core to 1830 ± 40 kilometers. The large core implies a martian mantle mineralogically similar to the terrestrial upper mantle and transition zone but differing from Earth by not having a bridgmanite-dominated lower mantle. We inferred a mean core density of 5.7 to 6.3 grams per cubic centimeter, which requires a substantial complement of light elements dissolved in the iron-nickel core. The seismic core shadow as seen from InSight's location covers half the surface of Mars, including the majority of potentially active regions-e.g., Tharsis-possibly limiting the number of detectable marsquakes.
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Affiliation(s)
| | - Amir Khan
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland.,Physik-Institut, University of Zürich, Zürich, Switzerland
| | - W Bruce Banerdt
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Philippe Lognonné
- Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France
| | | | - Savas Ceylan
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland
| | - Mélanie Drilleau
- Institut Supérieur de l'Aéronautique et de l'Espace SUPAERO, Toulouse, France
| | | | - Raphaël F Garcia
- Institut Supérieur de l'Aéronautique et de l'Espace SUPAERO, Toulouse, France
| | - Quancheng Huang
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Doyeon Kim
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Vedran Lekic
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Henri Samuel
- Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France
| | | | - Nicholas Schmerr
- Department of Geology, University of Maryland, College Park, MD, USA
| | | | - Éléonore Stutzmann
- Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France
| | - Zongbo Xu
- Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France
| | - Daniele Antonangeli
- Sorbonne Université, Muséum National d'Histoire Naturelle, UMR CNRS 7590, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, IMPMC, Paris, France
| | | | - Paul M Davis
- Department of Earth, Planetary, and Space Sciences, University of California Los Angeles, Los Angeles, CA, USA
| | | | - Taichi Kawamura
- Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France
| | | | - Ross Maguire
- Department of Geology, University of Maryland, College Park, MD, USA
| | - Angela G Marusiak
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Mark P Panning
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Clément Perrin
- Laboratoire de Planétologie et Géodynamique (LPG), UMR CNRS 6112, Université de Nantes, Université d'Angers, France
| | | | | | | | | | - Éric Beucler
- Laboratoire de Planétologie et Géodynamique (LPG), UMR CNRS 6112, Université de Nantes, Université d'Angers, France
| | - John Clinton
- Swiss Seismological Service (SED), ETH Zürich, Zürich, Switzerland
| | - Nikolaj Dahmen
- Institute of Geophysics, ETH Zürich, Zürich, Switzerland
| | | | - Tamara Gudkova
- Schmidt Institute of Physics of the Earth RAS, Moscow, Russia
| | - Anna Horleston
- School of Earth Sciences, University of Bristol, Bristol, UK
| | - W Thomas Pike
- Department of Electrical and Electronic Engineering, Imperial College, London, UK
| | - Matthieu Plasman
- Université de Paris, Institut de physique du globe de Paris, CNRS, Paris, France
| | - Suzanne E Smrekar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
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Timing of oceans on Mars from shoreline deformation. Nature 2018; 555:643-646. [PMID: 29555993 DOI: 10.1038/nature26144] [Citation(s) in RCA: 72] [Impact Index Per Article: 12.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/01/2017] [Accepted: 01/25/2018] [Indexed: 11/08/2022]
Abstract
Widespread evidence points to the existence of an ancient Martian ocean. Most compelling are the putative ancient shorelines in the northern plains. However, these shorelines fail to follow an equipotential surface, and this has been used to challenge the notion that they formed via an early ocean and hence to question the existence of such an ocean. The shorelines' deviation from a constant elevation can be explained by true polar wander occurring after the formation of Tharsis, a volcanic province that dominates the gravity and topography of Mars. However, surface loading from the oceans can drive polar wander only if Tharsis formed far from the equator, and most evidence indicates that Tharsis formed near the equator, meaning that there is no current explanation for the shorelines' deviation from an equipotential that is consistent with our geophysical understanding of Mars. Here we show that variations in shoreline topography can be explained by deformation caused by the emplacement of Tharsis. We find that the shorelines must have formed before and during the emplacement of Tharsis, instead of afterwards, as previously assumed. Our results imply that oceans on Mars formed early, concurrent with the valley networks, and point to a close relationship between the evolution of oceans on Mars and the initiation and decline of Tharsis volcanism, with broad implications for the geology, hydrological cycle and climate of early Mars.
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Cole HM, Andrews-Hanna JC. The anatomy of a wrinkle ridge revealed in the wall of Melas Chasma, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2017; 122:889-900. [PMID: 31534880 PMCID: PMC6750226 DOI: 10.1002/2017je005274] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Wrinkle ridges are among the most common tectonic structures on the terrestrial planets, and provide important records of the history of planetary strain and geodynamics. The observed broad arches and superposed narrow wrinkles are thought to be the surface manifestation of blind thrust faults, which terminate in near-surface volcanic sequences and cause folding and layer-parallel shear. However, the subsurface tectonic architecture associated with the ridges remains a matter of debate. Here we present direct observations of a wrinkle ridge thrust fault where it has been exposed by erosion in the southern wall of Melas Chasma on Mars. The thrust fault has been made resistant to erosion, likely due to volcanic intrusion, such that later erosional widening of the trough exposed the fault plane as a 70 km-long ridge extending into the chasma. A plane fit to this ridge crest reveals a thrust fault with a dip of 13° (+8°, -7°) between 1 and 3.5 km depth below the plateau surface, with no evidence for listric character in this depth range. This dip is significantly lower than the commonly assumed value of 30°, which, if representative of other wrinkle ridges, indicates that global contraction on Mars may have been previously underestimated.
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Affiliation(s)
- Hank M. Cole
- Department of Geophysics, Colorado School of Mines, Golden CO 80401
| | - Jeffrey C. Andrews-Hanna
- Southwest Research Institute, Boulder, CO 80302
- now at the Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092
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Late Tharsis formation and implications for early Mars. Nature 2016; 531:344-7. [PMID: 26934230 DOI: 10.1038/nature17171] [Citation(s) in RCA: 62] [Impact Index Per Article: 7.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/16/2015] [Accepted: 01/27/2016] [Indexed: 11/08/2022]
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Keske AL, Hamilton CW, McEwen AS, Daubar IJ. Episodes of fluvial and volcanic activity in Mangala Valles, Mars. ICARUS 2015; 245:333-347. [PMID: 29176911 PMCID: PMC5701667 DOI: 10.1016/j.icarus.2014.09.040] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
A new mapping-based study of the 900-km-long Mangala Valles outflow system was motivated by the availability of new high-resolution images and continued debates about the roles of water and lava in outflow channels on Mars. This study uses photogeologic analysis, geomorphic surface mapping, cratering statistics, and relative stratigraphy. Results show that Mangala Valles underwent at least two episodes of fluvial activity and at least three episodes of volcanic activity during the Late Amazonian. The occurrence of scoured bedrock at the base of the mapped stratigraphy, in addition to evidence provided by crater retention ages, suggests that fluvial activity preceded the deposition of two of the volcanic units. Crater counts performed at 30 locations throughout the area have allowed us to construct the following timeline: (1) formation of Noachian Highlands and possible initial flooding event(s) before ~1 Ga, (2) emplacement of Tharsis lava flows in the valley from ~700 to 1000 Ma, (3) a megaflooding event at ~700-800 Ma sourced from Mangala Fossa, (4) valley fill by a sequence of lava flows sourced from Mangala Fossa ~400-500 Ma, (5) another megaflooding event from ~400 Ma, (6) a final phase of volcanism sourced from Mangala Fossa ~300-350 Ma, and (7) emplacement of eolian sedimentary deposits in the northern portion of the valley ~300 Ma. These results are consistent with alternating episodes of aqueous flooding and volcanism in the valles. This pattern of geologic activity is similar to that of other outflow systems, such as Kasei Valles, suggesting that there is a recurring, and perhaps coupled, nature of these processes on Mars.
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Affiliation(s)
- Amber L. Keske
- School of Earth and Space Exploration, Arizona State University, 201 E. Orange Mall, Tempe, AZ 85287, United States
| | | | - Alfred S. McEwen
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, United States
| | - Ingrid J. Daubar
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, United States
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Platz T, Byrne PK, Massironi M, Hiesinger H. Volcanism and tectonism across the inner solar system: an overview. ACTA ACUST UNITED AC 2014. [DOI: 10.1144/sp401.22] [Citation(s) in RCA: 41] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/04/2022]
Abstract
AbstractVolcanism and tectonism are the dominant endogenic means by which planetary surfaces change. This book, in general, and this overview, in particular, aim to encompass the broad range in character of volcanism, tectonism, faulting and associated interactions observed on planetary bodies across the inner solar system – a region that includes Mercury, Venus, Earth, the Moon, Mars and asteroids. The diversity and breadth of landforms produced by volcanic and tectonic processes are enormous, and vary across the inventory of inner solar system bodies. As a result, the selection of prevailing landforms and their underlying formational processes that are described and highlighted in this review are but a primer to the expansive field of planetary volcanism and tectonism. In addition to this extended introductory contribution, this Special Publication features 21 dedicated research articles about volcanic and tectonic processes manifest across the inner solar system. Those articles are summarized at the end of this review.
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Affiliation(s)
- T. Platz
- Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719-2395, USA
- Freie Universität Berlin, Institute of Geological Sciences, Planetary Sciences & Remote Sensing, Malteserstrasse 74-100, 12249 Berlin, Germany
| | - P. K. Byrne
- Lunar and Planetary Institute, Universities Space Research Association, 3600 Bay Area Boulevard, Houston, TX 77058, USA
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road NW, Washington, DC 20015-1305, USA
| | - M. Massironi
- Dipartimento di Geoscienze, Universita' degli Studi di Padova, via G. Gradenigo 6, 35131 Padova, Italy
| | - H. Hiesinger
- Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Wilhelm-Klemm-Strasse 10, 48149 Münster, Germany
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Andrews-Hanna JC, Lewis KW. Early Mars hydrology: 2. Hydrological evolution in the Noachian and Hesperian epochs. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003709] [Citation(s) in RCA: 94] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Wray JJ, Milliken RE, Dundas CM, Swayze GA, Andrews-Hanna JC, Baldridge AM, Chojnacki M, Bishop JL, Ehlmann BL, Murchie SL, Clark RN, Seelos FP, Tornabene LL, Squyres SW. Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003694] [Citation(s) in RCA: 121] [Impact Index Per Article: 9.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Šrámek O, Zhong S. Long-wavelength stagnant lid convection with hemispheric variation in lithospheric thickness: Link between Martian crustal dichotomy and Tharsis? ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2010je003597] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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10
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Hynek BM, Beach M, Hoke MRT. Updated global map of Martian valley networks and implications for climate and hydrologic processes. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003548] [Citation(s) in RCA: 312] [Impact Index Per Article: 22.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hoke MRT, Hynek BM. Roaming zones of precipitation on ancient Mars as recorded in valley networks. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003247] [Citation(s) in RCA: 61] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Monica R. T. Hoke
- Department of Astrophysical and Planetary ScienceUniversity of Colorado at Boulder Boulder Colorado USA
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado at Boulder Boulder Colorado USA
| | - Brian M. Hynek
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado at Boulder Boulder Colorado USA
- Department of Geological SciencesUniversity of Colorado at Boulder Boulder Colorado USA
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Watters WA, Zuber MT, Hager BH. Thermal perturbations caused by large impacts and consequences for mantle convection. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2007je002964] [Citation(s) in RCA: 81] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Williams JP, Nimmo F, Moore WB, Paige DA. The formation of Tharsis on Mars: What the line-of-sight gravity is telling us. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003050] [Citation(s) in RCA: 22] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Bleacher JE, Greeley R, Williams DA, Cave SR, Neukum G. Trends in effusive style at the Tharsis Montes, Mars, and implications for the development of the Tharsis province. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002873] [Citation(s) in RCA: 74] [Impact Index Per Article: 4.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Kronberg P, Hauber E, Grott M, Werner SC, Schäfer T, Gwinner K, Giese B, Masson P, Neukum G. Acheron Fossae, Mars: Tectonic rifting, volcanism, and implications for lithospheric thickness. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002780] [Citation(s) in RCA: 37] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Newsom HE, Crumpler LS, Reedy RC, Petersen MT, Newsom GC, Evans LG, Taylor GJ, Keller JM, Janes DM, Boynton WV, Kerry KE, Karunatillake S. Geochemistry of Martian soil and bedrock in mantled and less mantled terrains with gamma ray data from Mars Odyssey. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002680] [Citation(s) in RCA: 28] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hahn BC, McLennan SM, Taylor GJ, Boynton WV, Dohm JM, Finch MJ, Hamara DK, Janes DM, Karunatillake S, Keller JM, Kerry KE, Metzger AE, Williams RMS. Mars Odyssey Gamma Ray Spectrometer elemental abundances and apparent relative surface age: Implications for Martian crustal evolution. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002821] [Citation(s) in RCA: 23] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Keller JM, Boynton WV, Karunatillake S, Baker VR, Dohm JM, Evans LG, Finch MJ, Hahn BC, Hamara DK, Janes DM, Kerry KE, Newsom HE, Reedy RC, Sprague AL, Squyres SW, Starr RD, Taylor GJ, Williams RMS. Equatorial and midlatitude distribution of chlorine measured by Mars Odyssey GRS. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002679] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Taylor GJ, Stopar JD, Boynton WV, Karunatillake S, Keller JM, Brückner J, Wänke H, Dreibus G, Kerry KE, Reedy RC, Evans LG, Starr RD, Martel LMV, Squyres SW, Gasnault O, Maurice S, d'Uston C, Englert P, Dohm JM, Baker VR, Hamara D, Janes D, Sprague AL, Kim KJ, Drake DM, McLennan SM, Hahn BC. Variations in K/Th on Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002676] [Citation(s) in RCA: 30] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Knapmeyer M, Oberst J, Hauber E, Wählisch M, Deuchler C, Wagner R. Working models for spatial distribution and level of Mars' seismicity. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002708] [Citation(s) in RCA: 129] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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21
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Frey HV. Impact constraints on, and a chronology for, major events in early Mars history. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002449] [Citation(s) in RCA: 126] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Schulze-Makuch D, Dohm JM, Fairén AG, Baker VR, Fink W, Strom RG. Venus, Mars, and the ices on Mercury and the moon: astrobiological implications and proposed mission designs. ASTROBIOLOGY 2005; 5:778-95. [PMID: 16379531 DOI: 10.1089/ast.2005.5.778] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/05/2023]
Abstract
Venus and Mars likely had liquid water bodies on their surface early in the Solar System history. The surfaces of Venus and Mars are presently not a suitable habitat for life, but reservoirs of liquid water remain in the atmosphere of Venus and the subsurface of Mars, and with it also the possibility of microbial life. Microbial organisms may have adapted to live in these ecological niches by the evolutionary force of directional selection. Missions to our neighboring planets should therefore be planned to explore these potentially life-containing refuges and return samples for analysis. Sample return missions should also include ice samples from Mercury and the Moon, which may contain information about the biogenic material that catalyzed the early evolution of life on Earth (or elsewhere). To obtain such information, science-driven exploration is necessary through varying degrees of mission operation autonomy. A hierarchical mission design is envisioned that includes spaceborne (orbital), atmosphere (airborne), surface (mobile such as rover and stationary such as lander or sensor), and subsurface (e.g., ground-penetrating radar, drilling, etc.) agents working in concert to allow for sufficient mission safety and redundancy, to perform extensive and challenging reconnaissance, and to lead to a thorough search for evidence of life and habitability.
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Solomon SC, Aharonson O, Aurnou JM, Banerdt WB, Carr MH, Dombard AJ, Frey HV, Golombek MP, Hauck SA, Head JW, Jakosky BM, Johnson CL, McGovern PJ, Neumann GA, Phillips RJ, Smith DE, Zuber MT. New Perspectives on Ancient Mars. Science 2005; 307:1214-20. [PMID: 15731435 DOI: 10.1126/science.1101812] [Citation(s) in RCA: 225] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Mars was most active during its first billion years. The core, mantle, and crust formed within approximately 50 million years of solar system formation. A magnetic dynamo in a convecting fluid core magnetized the crust, and the global field shielded a more massive early atmosphere against solar wind stripping. The Tharsis province became a focus for volcanism, deformation, and outgassing of water and carbon dioxide in quantities possibly sufficient to induce episodes of climate warming. Surficial and near-surface water contributed to regionally extensive erosion, sediment transport, and chemical alteration. Deep hydrothermal circulation accelerated crustal cooling, preserved variations in crustal thickness, and modified patterns of crustal magnetization.
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Affiliation(s)
- Sean C Solomon
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA.
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Rodríguez JAP. Control of impact crater fracture systems on subsurface hydrology, ground subsidence, and collapse, Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002365] [Citation(s) in RCA: 36] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Schulze-Makuch D, Irwin LN, Lipps JH, LeMone D, Dohm JM, Fairén AG. Scenarios for the evolution of life on Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002430] [Citation(s) in RCA: 38] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Ferrill DA, Wyrick DY, Morris AP, Sims DW, Franklin NM. Dilational fault slip and pit chain formation on Mars. ACTA ACUST UNITED AC 2004. [DOI: 10.1130/1052-5173(2004)014<4:dfsapc>2.0.co;2] [Citation(s) in RCA: 72] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/30/2022]
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28
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Irwin RP. Geomorphology of Ma'adim Vallis, Mars, and associated paleolake basins. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002287] [Citation(s) in RCA: 117] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Cailleau B, Walter TR, Janle P, Hauber E. Modeling volcanic deformation in a regional stress field: Implications for the formation of graben structures on Alba Patera, Mars. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002135] [Citation(s) in RCA: 34] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | - Thomas R. Walter
- Marine Geology and Geophysics; Rosenstiel School of Marine and Atmospheric Science; Miami Florida USA
| | - Peter Janle
- Institute of Geosciences, Department of Geophysics; Kiel University; Kiel Germany
| | - Ernst Hauber
- Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR); Berlin Germany
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30
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Wilkins SJ. Cross faults in extensional settings: Stress triggering, displacement localization, and implications for the origin of blunt troughs at Valles Marineris, Mars. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je001968] [Citation(s) in RCA: 48] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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31
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Hynek BM. Explosive volcanism in the Tharsis region: Global evidence in the Martian geologic record. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002062] [Citation(s) in RCA: 182] [Impact Index Per Article: 8.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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32
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Ruiz J. Amplitude of heat flow variations on Mars from possible shoreline topography. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002084] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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34
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Hynek BM. Geologic setting and origin of Terra Meridiani hematite deposit on Mars. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2002je001891] [Citation(s) in RCA: 149] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Wilson L. Tharsis-radial graben systems as the surface manifestation of plume-related dike intrusion complexes: Models and implications. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001593] [Citation(s) in RCA: 173] [Impact Index Per Article: 7.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Zhong S. Effects of lithosphere on the long-wavelength gravity anomalies and their implications for the formation of the Tharsis rise on Mars. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001589] [Citation(s) in RCA: 43] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Dohm JM, Ferris JC, Baker VR, Anderson RC, Hare TM, Strom RG, Barlow NG, Tanaka KL, Klemaszewski JE, Scott DH. Ancient drainage basin of the Tharsis region, Mars: Potential source for outflow channel systems and putative oceans or paleolakes. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001468] [Citation(s) in RCA: 168] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Abstract
Over the past 30 years, the water-generated landforms and landscapes of Mars have been revealed in increasing detail by a succession of spacecraft missions. Recent data from the Mars Global Surveyor mission confirm the view that brief episodes of water-related activity, including glaciation, punctuated the geological history of Mars. The most recent of these episodes seems to have occurred within the past 10 million years. These new results are anomalous in regard to the prevailing view that the martian surface has been continuously extremely cold and dry, much as it is today, for the past 3.9 billion years. Interpretations of the new data are controversial, but explaining the anomalies in a consistent manner leads to potentially fruitful hypotheses for understanding the evolution of Mars in relation to Earth.
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Affiliation(s)
- V R Baker
- Department of Hydrology and Water Resources, University of Arizona, Tucson, Arizona 85721-0011, USA.
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Abstract
There is substantial evidence that the martian volatile inventory and climate have changed markedly throughout the planet's history. Clues come from areas as disparate as the history and properties of the deep interior, the composition of the crust and regolith, the morphology of the surface, composition of the present-day atmosphere, and the nature of the interactions between the upper atmosphere and the solar wind. We piece together the relevant observations into a coherent view of the evolution of the martian climate, focusing in particular on the observations that provide the strongest constraints.
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Affiliation(s)
- B M Jakosky
- Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, Colorado 80309-0392, USA.
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