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Abstract
Marsquakes excite seismic wavefield, allowing the Martian interior structures to be probed. However, the Martian seismic data recorded by InSight have a low signal-to-noise ratio, making the identification of marsquakes challenging. Here we use the Matched Filter technique and Benford’s Law to detect hitherto undetected events. Based on nine marsquake templates, we report 47 newly detected events, >90% of which are associated with the two high-quality events located beneath Cerberus Fossae. They occurred at all times of the Martian day, thus excluding the tidal modulation (e.g., Phobos) as their cause. We attribute the newly discovered, low-frequency, repetitive events to magma movement associated with volcanic activity in the upper mantle beneath Cerberus Fossae. The continuous seismicity suggests that Cerberus Fossae is seismically highly active and that the Martian mantle is mobile. The authors detect 47 hitherto unreported low-frequency marsquakes originating from Cerberus Fossae at all times of the Martian day. The matched filter technique confirms repetitive events implying that the Martian mantle is dynamically active.
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2
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Abstract
From the 2000s onwards, unprecedented space missions have brought about a wealth of novel investigations on the different aspects of space geomechanics. Such aspects are related to the exploratory activities such as drilling, sampling, coring, water extraction, anchoring, etc. So far, a whole range of constitutive research projects on the plate tectonics, morphology, volcanic activities and volatile content of planetary bodies have been implemented. Furthermore, various laboratory experiments on extraterrestrial samples and their artificial terrestrial simulants are continually conducted to obtain the physical and mechanical properties of the corresponding specimens. Today, with the space boom being steered by diverse space agencies, the incorporation of geomechanics into space exploration appreciably appears much needed. The primary objective of this article is to collate and integrate the up-to-date investigations related to the geomechanical applications in space technologies. Emphasis is given to the new and future applications such as planetary drilling and water extraction. The main impetus is to provide a comprehensive reference for geoscience scientists and astronauts to quickly become acquainted with the cutting-edge advancements in the area of space geomechanics. Moreover, this research study also elaborates on the operational constraints in space geomechanics which necessitate further scientific investigations.
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3
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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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4
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Affiliation(s)
- Sanne Cottaar
- Department of Earth Sciences, University of Cambridge, Cambridge, UK.
| | - Paula Koelemeijer
- Department of Earth Sciences, Royal Holloway, University of London, Egham, UK
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5
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Kupenko I, Aprilis G, Vasiukov DM, McCammon C, Chariton S, Cerantola V, Kantor I, Chumakov AI, Rüffer R, Dubrovinsky L, Sanchez-Valle C. Magnetism in cold subducting slabs at mantle transition zone depths. Nature 2019; 570:102-106. [DOI: 10.1038/s41586-019-1254-8] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/02/2018] [Accepted: 04/01/2019] [Indexed: 11/09/2022]
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6
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Warner N, Gupta S, Lin SY, Kim JR, Muller JP, Morley J. Late Noachian to Hesperian climate change on Mars: Evidence of episodic warming from transient crater lakes near Ares Vallis. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003522] [Citation(s) in RCA: 45] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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7
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Grott M, Breuer D. On the spatial variability of the Martian elastic lithosphere thickness: Evidence for mantle plumes? ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003456] [Citation(s) in RCA: 62] [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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8
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Affiliation(s)
- Moira Jardine
- Department of Physics and Astronomy, University of St. Andrews, St. Andrews, KY16 9SS, UK.
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9
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The Mars Astrobiology Explorer-Cacher (MAX-C): a potential rover mission for 2018. Final report of the Mars Mid-Range Rover Science Analysis Group (MRR-SAG) October 14, 2009. ASTROBIOLOGY 2010; 10:127-163. [PMID: 20298148 DOI: 10.1089/ast.2010.0462] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
This report documents the work of the Mid-Range Rover Science Analysis Group (MRR-SAG), which was assigned to formulate a concept for a potential rover mission that could be launched to Mars in 2018. Based on programmatic and engineering considerations as of April 2009, our deliberations assumed that the potential mission would use the Mars Science Laboratory (MSL) sky-crane landing system and include a single solar-powered rover. The mission would also have a targeting accuracy of approximately 7 km (semimajor axis landing ellipse), a mobility range of at least 10 km, and a lifetime on the martian surface of at least 1 Earth year. An additional key consideration, given recently declining budgets and cost growth issues with MSL, is that the proposed rover must have lower cost and cost risk than those of MSL--this is an essential consideration for the Mars Exploration Program Analysis Group (MEPAG). The MRR-SAG was asked to formulate a mission concept that would address two general objectives: (1) conduct high priority in situ science and (2) make concrete steps toward the potential return of samples to Earth. The proposed means of achieving these two goals while balancing the trade-offs between them are described here in detail. We propose the name Mars Astrobiology Explorer-Cacher(MAX-C) to reflect the dual purpose of this potential 2018 rover mission.
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Bowles JA, Hammer JE, Brachfeld SA. Magnetic and petrologic characterization of synthetic Martian basalts and implications for the surface magnetization of Mars. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003378] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Julie A. Bowles
- Department of Geology and Geophysics; University of Hawai‘i at Mānoa; Honolulu Hawaii USA
| | - Julia E. Hammer
- Department of Geology and Geophysics; University of Hawai‘i at Mānoa; Honolulu Hawaii USA
| | - Stefanie A. Brachfeld
- Department of Earth and Environmental Studies; Montclair State University; Upper Montclair New Jersey USA
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11
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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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12
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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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13
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Terada N, Kulikov YN, Lammer H, Lichtenegger HIM, Tanaka T, Shinagawa H, Zhang T. Atmosphere and water loss from early Mars under extreme solar wind and extreme ultraviolet conditions. ASTROBIOLOGY 2009; 9:55-70. [PMID: 19216683 DOI: 10.1089/ast.2008.0250] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
The upper limits of the ion pickup and cold ion outflow loss rates from the early martian atmosphere shortly after the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) were investigated. We applied a comprehensive 3-D multi-species magnetohydrodynamic (MHD) model to an early martian CO(2)-rich atmosphere, which was assumed to have been exposed to a solar XUV [X-ray and extreme ultraviolet (EUV)] flux that was 100 times higher than today and a solar wind that was about 300 times denser. We also assumed the late onset of a planetary magnetic dynamo, so that Mars had no strong intrinsic magnetic field at that early period. We found that, due to such extreme solar wind-atmosphere interaction, a strong magnetic field of about approximately 4000 nT was induced in the entire dayside ionosphere, which could efficiently protect the upper atmosphere from sputtering loss. A planetary obstacle ( approximately ionopause) was formed at an altitude of about 1000 km above the surface due to the drag force and the mass loading by newly created ions in the highly extended upper atmosphere. We obtained an O(+) loss rate by the ion pickup process, which takes place above the ionopause, of about 1.5 x 10(28) ions/s during the first < or =150 million years, which is about 10(4) times greater than today and corresponds to a water loss equivalent to a global martian ocean with a depth of approximately 8 m. Consequently, even if the magnetic protection due to the expected early martian magnetic dynamo is neglected, ion pickup and sputtering were most likely not the dominant loss processes for the planet's initial atmosphere and water inventory. However, it appears that the cold ion outflow into the martian tail, due to the transfer of momentum from the solar wind to the ionospheric plasma, could have removed a global ocean with a depth of 10-70 m during the first < or =150 million years after the Sun arrived at the ZAMS.
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Affiliation(s)
- Naoki Terada
- National Institute of Information and Communications Technology, Tokyo, Japan.
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14
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Leblanc F, Langlais B, Fouchet T, Barabash S, Breuer D, Chassefière E, Coates A, Dehant V, Forget F, Lammer H, Lewis S, Lopez-Valverde M, Mandea M, Menvielle M, Pais A, Paetzold M, Read P, Sotin C, Tarits P, Vennerstrom S. Mars environment and magnetic orbiter scientific and measurement objectives. ASTROBIOLOGY 2009; 9:71-89. [PMID: 19317625 DOI: 10.1089/ast.2007.0222] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
In this paper, we summarize our present understanding of Mars' atmosphere, magnetic field, and surface and address past evolution of these features. Key scientific questions concerning Mars' surface, atmosphere, and magnetic field, along with the planet's interaction with solar wind, are discussed. We also define what key parameters and measurements should be performed and the main characteristics of a martian mission that would help to provide answers to these questions. Such a mission--Mars Environment and Magnetic Orbiter (MEMO)--was proposed as an answer to the Cosmic Vision Call of Opportunity as an M-class mission (corresponding to a total European Space Agency cost of less than 300 Meuro). MEMO was designed to study the strong interconnection between the planetary interior, atmosphere, and solar conditions, which is essential to our understanding of planetary evolution, the appearance of life, and its sustainability. The MEMO main platform combined remote sensing and in situ measurements of the atmosphere and the magnetic field during regular incursions into the martian upper atmosphere. The micro-satellite was designed to perform simultaneous in situ solar wind measurements. MEMO was defined to conduct: * Four-dimensional mapping of the martian atmosphere from the surface up to 120 km by measuring wind, temperature, water, and composition, all of which would provide a complete view of the martian climate and photochemical system; Mapping of the low-altitude magnetic field with unprecedented geographical, altitude, local time, and seasonal resolutions; A characterization of the simultaneous responses of the atmosphere, magnetic field, and near-Mars space to solar variability by means of in situ atmospheric and solar wind measurements.
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Affiliation(s)
- F Leblanc
- Service d'Aéronomie du CNRS/IPSL, Université Pierre et Marie Curie, France.
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15
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Silvers LJ. Magnetic fields in astrophysical objects. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2008; 366:4453-4464. [PMID: 18812299 DOI: 10.1098/rsta.2008.0173] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/26/2023]
Abstract
Magnetic fields are known to reside in many astrophysical objects and are now believed to be crucially important for the creation of phenomena on a wide variety of scales. However, the role of the magnetic field in the bodies that we observe has not always been clear. In certain situations, the importance of a magnetic field has been overlooked on the grounds that the large-scale magnetic field was believed to be too weak to play an important role in the dynamics. In this article I discuss some of the recent developments concerning magnetic fields in stars, planets and accretion discs. I choose to emphasize some of the situations where it has been suggested that weak magnetic fields may play a more significant role than previously thought. At the end of the article, I list some of the questions to be answered in the future.
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Affiliation(s)
- L J Silvers
- Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Wilberforce Road, Cambridge, UK.
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16
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Jellinek AM, Johnson CL, Schubert G. Constraints on the elastic thickness, heat flow, and melt production at early Tharsis from topography and magnetic field observations. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003005] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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17
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Khan A, Connolly JAD. Constraining the composition and thermal state of Mars from inversion of geophysical data. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002996] [Citation(s) in RCA: 68] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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18
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Arkani-Hamed J, Seyed-Mahmoud B, Aldridge KD, Baker RE. Tidal excitation of elliptical instability in the Martian core: Possible mechanism for generating the core dynamo. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002982] [Citation(s) in RCA: 22] [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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19
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Chaufray JY, Modolo R, Leblanc F, Chanteur G, Johnson RE, Luhmann JG. Mars solar wind interaction: Formation of the Martian corona and atmospheric loss to space. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002915] [Citation(s) in RCA: 101] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Abstract
The evolution of the martian core is widely assumed to mirror the characteristics observed for Earth's core. Data from experiments performed on iron-sulfur and iron-nickel-sulfur systems at pressures corresponding to the center of Mars indicate that its core is presently completely liquid and that it will not form an outwardly crystallizing iron-rich inner core, as does Earth. Instead, planetary cooling will lead to core crystallization following either a "snowing-core" model, whereby iron-rich solids nucleate in the outer portions of the core and sink toward the center, or a "sulfide inner-core" model, where an iron-sulfide phase crystallizes to form a solid inner core.
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Affiliation(s)
- Andrew J Stewart
- Institute for Mineralogy and Petrology, Eidgenössische Technische Hochschule Zurich, CH 8092 Zurich, Switzerland
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21
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Tarduno JA, Cottrell RD, Watkeys MK, Bauch D. Geomagnetic field strength 3.2 billion years ago recorded by single silicate crystals. Nature 2007; 446:657-60. [PMID: 17410173 DOI: 10.1038/nature05667] [Citation(s) in RCA: 99] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/30/2006] [Accepted: 02/07/2007] [Indexed: 11/08/2022]
Abstract
The strength of the Earth's early geomagnetic field is of importance for understanding the evolution of the Earth's deep interior, surface environment and atmosphere. Palaeomagnetic and palaeointensity data from rocks formed near the boundary of the Proterozoic and Archaean eons, some 2.5 Gyr ago, show many hallmarks of the more recent geomagnetic field. Reversals are recorded, palaeosecular variation data indicate a dipole-dominated morphology and available palaeointensity values are similar to those from younger rocks. The picture before 2.8 Gyr ago is much less clear. Rocks of the Archaean Kaapvaal craton (South Africa) are among the best-preserved, but even they have experienced low-grade metamorphism. The variable acquisition of later magnetizations by these rocks is therefore expected, precluding use of conventional palaeointensity methods. Silicate crystals from igneous rocks, however, can contain minute magnetic inclusions capable of preserving Archaean-age magnetizations. Here we use a CO2 laser heating approach and direct-current SQUID magnetometer measurements to obtain palaeodirections and intensities from single silicate crystals that host magnetite inclusions. We find 3.2-Gyr-old field strengths that are within 50 per cent of the present-day value, indicating that a viable magnetosphere sheltered the early Earth's atmosphere from solar wind erosion.
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Affiliation(s)
- John A Tarduno
- Department of Earth and Environmental Sciences, University of Rochester, Rochester, New York 14627, USA.
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22
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Parmentier EM, Zuber MT. Early evolution of Mars with mantle compositional stratification or hydrothermal crustal cooling. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2005je002626] [Citation(s) in RCA: 39] [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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23
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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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24
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Ke Y, Solomatov VS. Early transient superplumes and the origin of the Martian crustal dichotomy. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002631] [Citation(s) in RCA: 40] [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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25
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Affiliation(s)
- Yingwei Fei
- Geophysical Laboratory, Carnegie Institution of Washington, Washington, DC 20015, USA.
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26
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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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27
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28
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Harrison KP. Groundwater-controlled valley networks and the decline of surface runoff on early Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002455] [Citation(s) in RCA: 75] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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29
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Affiliation(s)
- B. Langlais
- NAS/NRC at Geodynamics Branch; NASA Goddard Space Flight Center; Greenbelt Maryland USA
| | - M. E. Purucker
- Raytheon ITSS at Geodynamics Branch; NASA Goddard Space Flight Center; Greenbelt Maryland USA
| | - M. Mandea
- Institut de Physique du Globe; Paris France
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31
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Murthy VR, van Westrenen W, Fei Y. Experimental evidence that potassium is a substantial radioactive heat source in planetary cores. Nature 2003; 423:163-5. [PMID: 12736683 DOI: 10.1038/nature01560] [Citation(s) in RCA: 156] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/28/2002] [Accepted: 03/07/2003] [Indexed: 11/09/2022]
Abstract
The hypothesis that (40)K may be a significant radioactive heat source in the Earth's core was proposed on theoretical grounds over three decades ago, but experiments have provided only ambiguous and contradictory evidence for the solubility of potassium in iron-rich alloys. The existence of such radioactive heat in the core would have important implications for our understanding of the thermal evolution of the Earth and global processes such as the generation of the geomagnetic field, the core-mantle boundary heat flux and the time of formation of the inner core. Here we provide experimental evidence to show that the ambiguous results obtained from earlier experiments are probably due to previously unrecognized experimental and analytical difficulties. The high-pressure, high-temperature data presented here show conclusively that potassium enters iron sulphide melts in a strongly temperature-dependent fashion and that (40)K can serve as a substantial heat source in the cores of the Earth and Mars.
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Affiliation(s)
- V Rama Murthy
- Department of Geology and Geophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA.
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32
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Balog PS, Secco RA, Rubie DC, Frost DJ. Equation of state of liquid Fe-10 wt % S: Implications for the metallic cores of planetary bodies. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2001jb001646] [Citation(s) in RCA: 63] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- P. S. Balog
- Department of Earth Sciences; University of Western Ontario; London Ontario Canada
| | - R. A. Secco
- Department of Earth Sciences; University of Western Ontario; London Ontario Canada
| | - D. C. Rubie
- Bayerisches Geoinstitut; Universität Bayreuth; Bayreuth Germany
| | - D. J. Frost
- Bayerisches Geoinstitut; Universität Bayreuth; Bayreuth Germany
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Stegman DR, Jellinek AM, Zatman SA, Baumgardner JR, Richards MA. An early lunar core dynamo driven by thermochemical mantle convection. Nature 2003; 421:143-6. [PMID: 12520295 DOI: 10.1038/nature01267] [Citation(s) in RCA: 149] [Impact Index Per Article: 7.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/25/2002] [Accepted: 10/25/2002] [Indexed: 11/10/2022]
Abstract
Although the Moon currently has no internally generated magnetic field, palaeomagnetic data, combined with radiometric ages of Apollo samples, provide evidence for such a magnetic field from approximately 3.9 to 3.6 billion years (Gyr) ago, possibly owing to an ancient lunar dynamo. But the presence of a lunar dynamo during this time period is difficult to explain, because thermal evolution models for the Moon yield insufficient core heat flux to power a dynamo after approximately 4.2 Gyr ago. Here we show that a transient increase in core heat flux after an overturn of an initially stratified lunar mantle might explain the existence and timing of an early lunar dynamo. Using a three-dimensional spherical convection model, we show that a dense layer, enriched in radioactive elements (a 'thermal blanket'), at the base of the lunar mantle can initially prevent core cooling, thereby inhibiting core convection and magnetic field generation. Subsequent radioactive heating progressively increases the buoyancy of the thermal blanket, ultimately causing it to rise back into the mantle. The removal of the thermal blanket, proposed to explain the eruption of thorium- and titanium-rich lunar mare basalts, plausibly results in a core heat flux sufficient to power a short-lived lunar dynamo.
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Affiliation(s)
- Dave R Stegman
- Department of Earth and Planetary Science, University of California, Berkeley, California 94720, USA.
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Breuer D. Early plate tectonics versus single-plate tectonics on Mars: Evidence from magnetic field history and crust evolution. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je001999] [Citation(s) in RCA: 175] [Impact Index Per Article: 8.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Arkani-Hamed J, Riendler L. Stress differences in the Martian lithosphere: Constraints on the thermal state of Mars. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2002je001851] [Citation(s) in RCA: 12] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | - Lucas Riendler
- Earth and Planetary Sciences; McGill University; Montreal Quebec Canada
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Abstract
AbstractThe tectonic evolution of Archaean granite-greenstone terranes remains controversial. Here this subject is reviewed and illustrated with new data from the Slave craton. These data show that a thick, c. 2.7Ga, pillow basalt sequences extruded across extended sialic basement of the Slave craton at a scale comparable with that of modern large igneous provinces. The pillow basalts do not represent obducted oceanic allochthons. Basement-cover relationships argue for autochthonous to parautochthonous development of the basaltic greenstone belts of the west-central Slave craton, an interpretation that is further supported by geochemical and geochronological data. Similar data exist for several other cratons and granite-greenstone terrains, including the Abitibi greenstone belt of the Superior craton, where stratigraphic and subtle zircon inheritance data are equally incompatible with accretion of oceanic allochthons. Many classical granite-greenstone terrains, including most well-documented komatiite occurrences, thus appear to have formed in extensional environments within or on the margins of older continental crust. Closest modern analogues for such basalt-komatiite-rhyolite-dominated greenstone successions are rifts, marginal basins and volcanic rifted margins. Indeed, these environments have high preservation potential compared with fully oceanic settings. Collapse and structural telescoping of these highly extended volcano-sedimentary basins would allow for the complex structural development seen in granite-greenstone terrains while maintaining broadly autochthonous to parautochthonous tectonostratigraphic relationships. Seismic reflection profiles cannot discriminate between these telescoped autochthonous to parautochthonous settings and truly allochthonous accretionary complexes. Only carefully constructed structural-stratigraphic cross-sections, allowing some degree of palinspastic reconstruction, and underpinned by sufficient U-Pb zircon dating, can address the degree of allochthoneity of greenstone packages. Furthermore, seismic reflection profiles are essentially blind for the steep structures produced by multiple phases of upright folding and buoyant rise of mid- to lower-crustal, composite, granitoid and gneiss domes. Such structures are ubiquitous in granite-greenstone terrains and, indeed, most of these terrains appear to have experienced at least one phase of convective overturn to re-establish a stable density configuration, irrespective of the complexities of the pre-doming structural history. Buoyant rise of mid- to lower-crustal granitoid and gneiss domes can explain the typical size and spacing characteristics of such domes in granite-greenstone terranes, and the coeval deposition of late-kinematic, ‘Timiskaming-type’ conglomerate-sandstone successions in flanking basins. The extensional and subsequent contractional evolution of granite-greenstone terrains may have occurred in the overall context of a plate tectonic regime (e.g. volcanic rifted margins, back-arc basins) but highly extended, intraplate, rift-like settings seem equally plausible. Explaining the evolution of the latter in terms of Wilson cycles is misguided. Periods of intense rifting and flood volcanism (e.g. 2.73–2.70 Ga) may have been related to increased mantle plume activity or perhaps catastrophic mantle overturn events. Although there is evidence for plate-like lateral movement in late Archaean time (e.g. lateral heterogeneity of cratons, arc-like volcanism, cratonscale deformation patterns, strike-slip faults, etc.), the details of how these plate-like crustal blocks interacted and how they responded to rifting and collision appear to have differed significantly from those in Phanerozoic time. The most productive approach for Archaean research is probably to more fully understand and quantify these differences rather than the common emphasis on the superficial similarities with modern plate tectonics.
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Affiliation(s)
- Wouter Bleeker
- Continental Geoscience Division, Geological Survey of Canada
601 Booth Street, Ottawa, Ontario K1A 0E8, Canada
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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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Smith DE, Zuber MT, Frey HV, Garvin JB, Head JW, Muhleman DO, Pettengill GH, Phillips RJ, Solomon SC, Zwally HJ, Banerdt WB, Duxbury TC, Golombek MP, Lemoine FG, Neumann GA, Rowlands DD, Aharonson O, Ford PG, Ivanov AB, Johnson CL, McGovern PJ, Abshire JB, Afzal RS, Sun X. Mars Orbiter Laser Altimeter: Experiment summary after the first year of global mapping of Mars. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001364] [Citation(s) in RCA: 1152] [Impact Index Per Article: 50.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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