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The impact origin and evolution of Chryse Planitia on Mars revealed by buried craters. Nat Commun 2019; 10:4257. [PMID: 31534129 PMCID: PMC6751168 DOI: 10.1038/s41467-019-12162-0] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/07/2019] [Accepted: 07/31/2019] [Indexed: 11/08/2022] Open
Abstract
Large impacts are one of the most important processes shaping a planet's surface. On Mars, the early formation of the Martian crust and the lack of large impact basins (only four unambiguously identified: Hellas, Argyre, Utopia, and Isidis) indicates that a large part of early records of Mars' impact history is missing. Here we show, in Chryse Planitia, the scarcity of buried impact craters in a near-circular area could be explained by a pre-existing topographic depression with more intense resurfacing. Spatially correlated with positive Bouguer anomaly, this near-circular region with a diameter of ~1090 km likely originated from an impact. This proposed large impact basin must have been quickly relaxed or buried after its formation more than 4.0 billion years ago and heavily modified by subsequent resurfacing events. We anticipate our study to open a new window to unravelling the buried records of early Martian bombardment record.
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2
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Abstract
Using viscoelastic mass spring model simulations to track heat distribution inside a tidally perturbed body, we measure the near/far side asymmetry of heating in the crust of a spin synchronous Moon in eccentric orbit about the Earth. With the young Moon within. 8 Earth radii of the Earth, we find that tidal heating per unit area in a lunar crustal shell is asymmetric due to the octupole order moment in the Earth's tidal field and is 10 to 20% higher on its near side than on its far side. Tidal heating reduces the crustal basal heat flux and the rate of magma ocean crystallization. Assuming that the local crustal growth rate depends on the local basal heat flux and the distribution of tidal heating in latitude and longitude, a heat conductivity model illustrates that a moderately asymmetric and growing lunar crust could maintain its near/far side thickness asymmetry but only while the Moon is near the Earth.
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Affiliation(s)
- Alice C Quillen
- Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA
| | - Larkin Martini
- Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA
- Department of Geology and Geological Engineering, Colorado School of Mines, Golden, CO 80401, USA
| | - Miki Nakajima
- Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA
- Department of Earth and Environmental Sciences, University of Rochester, Rochester, NY 14627, USA
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3
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Andrews-Hanna JC, Head JW, Johnson B, Keane JT, Kiefer WS, McGovern PJ, Neumann GA, Wieczorek MA, Zuber MT. Ring faults and ring dikes around the Orientale basin on the Moon. ICARUS 2018; 310:1-20. [PMID: 29755136 PMCID: PMC5939591 DOI: 10.1016/j.icarus.2017.12.012] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/30/2023]
Abstract
The Orientale basin is the youngest and best-preserved multiring impact basin on the Moon, having experienced only modest modification by subsequent impacts and volcanism. Orientale is often treated as the type example of a multiring basin, with three prominent rings outside of the inner depression: the Inner Rook Montes, the Outer Rook Montes, and the Cordillera. Here we use gravity data from NASA's Gravity Recovery and Interior Laboratory (GRAIL) mission to reveal the subsurface structure of Orientale and its ring system. Gradients of the gravity data reveal a continuous ring dike intruded into the Outer Rook along the plane of the fault associated with the ring scarp. The volume of this ring dike is ~18 times greater than the volume of all extrusive mare deposits associated with the basin. The gravity gradient signature of the Cordillera ring indicates an offset along the fault across a shallow density interface, interpreted to be the base of the low-density ejecta blanket. Both gravity gradients and crustal thickness models indicate that the edge of the central cavity is shifted inward relative to the equivalent Inner Rook ring at the surface. Models of the deep basin structure show inflections along the crust-mantle interface at both the Outer Rook and Cordillera rings, indicating that the basin ring faults extend from the surface to at least the base of the crust. Fault dips range from 13-22° for the Cordillera fault in the northeastern quadrant, to 90° for the Outer Rook in the northwestern quadrant. The fault dips for both outer rings are lowest in the northeast, possibly due to the effects of either the direction of projectile motion or regional gradients in pre-impact crustal thickness. Similar ring dikes and ring faults are observed around the majority of lunar basins.
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Affiliation(s)
| | - James W Head
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - Brandon Johnson
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - James T Keane
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - Walter S Kiefer
- Lunar and Planetary Institute, University Space Research Association, Houston, TX 77058, USA
| | - Patrick J McGovern
- Lunar and Planetary Institute, University Space Research Association, Houston, TX 77058, USA
| | - Gregory A Neumann
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Mark A Wieczorek
- Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, France
| | - Maria T Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA
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4
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The Influence of a Substellar Continent on the Climate of a Tidally Locked Exoplanet. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aaad0a] [Citation(s) in RCA: 34] [Impact Index Per Article: 5.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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5
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Thermal Analysis of the Driving Component Based on the Thermal Network Method in a Lunar Drilling System and Experimental Verification. ENERGIES 2017. [DOI: 10.3390/en10030355] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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6
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Zuber MT, Smith DE, Neumann GA, Goossens S, Andrews-Hanna JC, Head JW, Kiefer WS, Asmar SW, Konopliv AS, Lemoine FG, Matsuyama I, Melosh HJ, McGovern PJ, Nimmo F, Phillips RJ, Solomon SC, Taylor GJ, Watkins MM, Wieczorek MA, Williams JG, Jansen JC, Johnson BC, Keane JT, Mazarico E, Miljković K, Park RS, Soderblom JM, Yuan DN. Gravity field of the Orientale basin from the Gravity Recovery and Interior Laboratory Mission. Science 2016; 354:438-441. [PMID: 27789835 PMCID: PMC7462089 DOI: 10.1126/science.aag0519] [Citation(s) in RCA: 26] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/05/2016] [Accepted: 09/16/2016] [Indexed: 11/02/2022]
Abstract
The Orientale basin is the youngest and best-preserved major impact structure on the Moon. We used the Gravity Recovery and Interior Laboratory (GRAIL) spacecraft to investigate the gravitational field of Orientale at 3- to 5-kilometer (km) horizontal resolution. A volume of at least (3.4 ± 0.2) × 106 km3 of crustal material was removed and redistributed during basin formation. There is no preserved evidence of the transient crater that would reveal the basin's maximum volume, but its diameter may now be inferred to be between 320 and 460 km. The gravity field resolves distinctive structures of Orientale's three rings and suggests the presence of faults associated with the outer two that penetrate to the mantle. The crustal structure of Orientale provides constraints on the formation of multiring basins.
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Affiliation(s)
- Maria T Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA.
| | - David E Smith
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA
| | - Gregory A Neumann
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Sander Goossens
- Center for Research and Exploration in Space Science and Technology, University of Maryland, Baltimore County, Baltimore, MD 21250, USA
| | - Jeffrey C Andrews-Hanna
- Department of Geophysics and Center for Space Resources, Colorado School of Mines, Golden, CO 80401, USA. Southwest Research Institute, Boulder, CO 80302, USA
| | - James W Head
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | | | - Sami W Asmar
- Jet Propulsion Laboratory, Pasadena, CA 91109, USA
| | | | - Frank G Lemoine
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Isamu Matsuyama
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, USA
| | - H Jay Melosh
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN 47907, USA
| | | | - Francis Nimmo
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, Santa Cruz, CA 95064, USA
| | | | - Sean C Solomon
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA. Lamont-Doherty Earth Observatory, Columbia University, Palisades, NY 10964, USA
| | - G Jeffrey Taylor
- Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
| | - Michael M Watkins
- Jet Propulsion Laboratory, Pasadena, CA 91109, USA. Center for Space Research, University of Texas, Austin, TX 78712 USA
| | - Mark A Wieczorek
- Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, 75205 Paris Cedex 13, France
| | | | - Johanna C Jansen
- Department of Geophysics and Center for Space Resources, Colorado School of Mines, Golden, CO 80401, USA
| | - Brandon C Johnson
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA. Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - James T Keane
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092, USA
| | - Erwan Mazarico
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Katarina Miljković
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA. Department of Applied Geology, Curtin University, Perth, Western Australia 6845, Australia
| | - Ryan S Park
- Jet Propulsion Laboratory, Pasadena, CA 91109, USA
| | - Jason M Soderblom
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA
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7
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Neumann GA, Zuber MT, Wieczorek MA, Head JW, Baker DMH, Solomon SC, Smith DE, Lemoine FG, Mazarico E, Sabaka TJ, Goossens SJ, Melosh HJ, Phillips RJ, Asmar SW, Konopliv AS, Williams JG, Sori MM, Soderblom JM, Miljković K, Andrews-Hanna JC, Nimmo F, Kiefer WS. Lunar impact basins revealed by Gravity Recovery and Interior Laboratory measurements. SCIENCE ADVANCES 2015; 1:e1500852. [PMID: 26601317 PMCID: PMC4646831 DOI: 10.1126/sciadv.1500852] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/26/2015] [Accepted: 08/18/2015] [Indexed: 05/30/2023]
Abstract
Observations from the Gravity Recovery and Interior Laboratory (GRAIL) mission indicate a marked change in the gravitational signature of lunar impact structures at the morphological transition, with increasing diameter, from complex craters to peak-ring basins. At crater diameters larger than ~200 km, a central positive Bouguer anomaly is seen within the innermost peak ring, and an annular negative Bouguer anomaly extends outward from this ring to the outer topographic rim crest. These observations demonstrate that basin-forming impacts remove crustal materials from within the peak ring and thicken the crust between the peak ring and the outer rim crest. A correlation between the diameter of the central Bouguer gravity high and the outer topographic ring diameter for well-preserved basins enables the identification and characterization of basins for which topographic signatures have been obscured by superposed cratering and volcanism. The GRAIL inventory of lunar basins improves upon earlier lists that differed in their totals by more than a factor of 2. The size-frequency distributions of basins on the nearside and farside hemispheres of the Moon differ substantially; the nearside hosts more basins larger than 350 km in diameter, whereas the farside has more smaller basins. Hemispherical differences in target properties, including temperature and porosity, are likely to have contributed to these different distributions. Better understanding of the factors that control basin size will help to constrain models of the original impactor population.
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Affiliation(s)
- Gregory A. Neumann
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Maria T. Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Mark A. Wieczorek
- Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, CNRS, Paris 75013, France
| | - James W. Head
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - David M. H. Baker
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - Sean C. Solomon
- Lamont-Doherty Earth Observatory, Columbia University, Palisades, NY 10964, USA
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | - David E. Smith
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Frank G. Lemoine
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Erwan Mazarico
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Terence J. Sabaka
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Sander J. Goossens
- Center for Research and Exploration in Space Science and Technology, University of Maryland, Baltimore County, Baltimore, MD 21250, USA
| | - H. Jay Melosh
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN 47907, USA
| | - Roger J. Phillips
- Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302, USA
| | - Sami W. Asmar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109–8099, USA
| | - Alexander S. Konopliv
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109–8099, USA
| | - James G. Williams
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109–8099, USA
| | - Michael M. Sori
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Jason M. Soderblom
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Katarina Miljković
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Jeffrey C. Andrews-Hanna
- Department of Geophysics and Center for Space Resources, Colorado School of Mines, Golden, CO 80401, USA
| | - Francis Nimmo
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, Santa Cruz, CA 95064, USA
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8
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Abstract
The inductive generation of magnetic fields in fluid planetary interiors is known as the dynamo process. Although the Moon today has no global magnetic field, it has been known since the Apollo era that the lunar rocks and crust are magnetized. Until recently, it was unclear whether this magnetization was the product of a core dynamo or fields generated externally to the Moon. New laboratory and spacecraft measurements strongly indicate that much of this magnetization is the product of an ancient core dynamo. The dynamo field persisted from at least 4.25 to 3.56 billion years ago (Ga), with an intensity reaching that of the present Earth. The field then declined by at least an order of magnitude by ∼3.3 Ga. The mechanisms for sustaining such an intense and long-lived dynamo are uncertain but may include mechanical stirring by the mantle and core crystallization.
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Affiliation(s)
- Benjamin P Weiss
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA.
| | - Sonia M Tikoo
- Department of Earth and Planetary Science, University of California, Berkeley, CA 94720, USA. Berkeley Geochronology Center, 2455 Ridge Road, Berkeley, CA 94709, USA
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9
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Garrick-Bethell I, Perera V, Nimmo F, Zuber MT. The tidal-rotational shape of the Moon and evidence for polar wander. Nature 2014; 512:181-4. [PMID: 25079322 DOI: 10.1038/nature13639] [Citation(s) in RCA: 48] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/27/2014] [Accepted: 07/01/2014] [Indexed: 11/09/2022]
Abstract
The origin of the Moon's large-scale topography is important for understanding lunar geology, lunar orbital evolution and the Moon's orientation in the sky. Previous hypotheses for its origin have included late accretion events, large impacts, tidal effects and convection processes. However, testing these hypotheses and quantifying the Moon's topography is complicated by the large basins that have formed since the crust crystallized. Here we estimate the large-scale lunar topography and gravity spherical harmonics outside these basins and show that the bulk of the spherical harmonic degree-2 topography is consistent with a crust-building process controlled by early tidal heating throughout the Moon. The remainder of the degree-2 topography is consistent with a frozen tidal-rotational bulge that formed later, at a semi-major axis of about 32 Earth radii. The probability of the degree-2 shape having both tidal-heating and frozen shape characteristics by chance is less than 1%. We also infer that internal density contrasts eventually reoriented the Moon's polar axis by 36 ± 4°, to the configuration we observe today. Together, these results link the geology of the near and far sides, and resolve long-standing questions about the Moon's large-scale shape, gravity and history of polar wander.
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Affiliation(s)
- Ian Garrick-Bethell
- 1] Department of Earth and Planetary Sciences, University of California, Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA [2] School of Space Research, Kyung Hee University, 1 Seocheon-dong, Giheung-gu, Yongin-si, Gyeonggi-do 446-701, Korea
| | - Viranga Perera
- 1] Department of Earth and Planetary Sciences, University of California, Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA [2] School of Earth and Space Exploration, Arizona State University, PO Box 876004, Tempe, Arizona 85287-6004, USA
| | - Francis Nimmo
- Department of Earth and Planetary Sciences, University of California, Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA
| | - Maria T Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, Massachusetts 02139, USA
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10
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Melosh HJ, Freed AM, Johnson BC, Blair DM, Andrews-Hanna JC, Neumann GA, Phillips RJ, Smith DE, Solomon SC, Wieczorek MA, Zuber MT. The origin of lunar mascon basins. Science 2013; 340:1552-5. [PMID: 23722426 DOI: 10.1126/science.1235768] [Citation(s) in RCA: 138] [Impact Index Per Article: 12.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
High-resolution gravity data from the Gravity Recovery and Interior Laboratory spacecraft have clarified the origin of lunar mass concentrations (mascons). Free-air gravity anomalies over lunar impact basins display bull's-eye patterns consisting of a central positive (mascon) anomaly, a surrounding negative collar, and a positive outer annulus. We show that this pattern results from impact basin excavation and collapse followed by isostatic adjustment and cooling and contraction of a voluminous melt pool. We used a hydrocode to simulate the impact and a self-consistent finite-element model to simulate the subsequent viscoelastic relaxation and cooling. The primary parameters controlling the modeled gravity signatures of mascon basins are the impactor energy, the lunar thermal gradient at the time of impact, the crustal thickness, and the extent of volcanic fill.
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Affiliation(s)
- H J Melosh
- Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, 550 Stadium Mall Drive, West Lafayette, IN 47907, USA.
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11
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Saberi AA. Percolation description of the global topography of Earth and the moon. PHYSICAL REVIEW LETTERS 2013; 110:178501. [PMID: 23679788 DOI: 10.1103/physrevlett.110.178501] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/13/2012] [Indexed: 06/02/2023]
Abstract
Remarkable global correlations exist between geometrical features of terrestrial surfaces on Earth, current mean sea level, and its geological internal processes whose origins have remained an essential goal in the earth sciences. Theoretical modeling of the ubiquitous self-similar fractal patterns observed on Earth and their underlying rules is indeed of great importance. Here I present a percolation description of the global topography of Earth in which the present mean sea level is automatically singled out as a critical level in the model. This finding elucidates the origins of the appearance of scale invariant patterns on Earth. The criticality is shown to be accompanied by a continental aggregation, unraveling an important correlation between the water and long-range topographic evolutions. To have a comparison point in hand, I apply such an analysis to the lunar topography which reveals various characteristic features of the Moon.
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Affiliation(s)
- Abbas Ali Saberi
- Department of Physics, College of Science, University of Tehran, P.O. Box 14395-547, Tehran, Iran.
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12
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Wieczorek MA, Neumann GA, Nimmo F, Kiefer WS, Taylor GJ, Melosh HJ, Phillips RJ, Solomon SC, Andrews-Hanna JC, Asmar SW, Konopliv AS, Lemoine FG, Smith DE, Watkins MM, Williams JG, Zuber MT. The crust of the Moon as seen by GRAIL. Science 2012; 339:671-5. [PMID: 23223394 DOI: 10.1126/science.1231530] [Citation(s) in RCA: 75] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
High-resolution gravity data obtained from the dual Gravity Recovery and Interior Laboratory (GRAIL) spacecraft show that the bulk density of the Moon's highlands crust is 2550 kilograms per cubic meter, substantially lower than generally assumed. When combined with remote sensing and sample data, this density implies an average crustal porosity of 12% to depths of at least a few kilometers. Lateral variations in crustal porosity correlate with the largest impact basins, whereas lateral variations in crustal density correlate with crustal composition. The low-bulk crustal density allows construction of a global crustal thickness model that satisfies the Apollo seismic constraints, and with an average crustal thickness between 34 and 43 kilometers, the bulk refractory element composition of the Moon is not required to be enriched with respect to that of Earth.
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Affiliation(s)
- Mark A Wieczorek
- Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, Case 7071, Lamarck A, 5, rue Thomas Mann, 75205 Paris Cedex 13, France.
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13
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Zuber MT, Smith DE, Watkins MM, Asmar SW, Konopliv AS, Lemoine FG, Melosh HJ, Neumann GA, Phillips RJ, Solomon SC, Wieczorek MA, Williams JG, Goossens SJ, Kruizinga G, Mazarico E, Park RS, Yuan DN. Gravity field of the Moon from the Gravity Recovery and Interior Laboratory (GRAIL) mission. Science 2012; 339:668-71. [PMID: 23223395 DOI: 10.1126/science.1231507] [Citation(s) in RCA: 317] [Impact Index Per Article: 26.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Spacecraft-to-spacecraft tracking observations from the Gravity Recovery and Interior Laboratory (GRAIL) have been used to construct a gravitational field of the Moon to spherical harmonic degree and order 420. The GRAIL field reveals features not previously resolved, including tectonic structures, volcanic landforms, basin rings, crater central peaks, and numerous simple craters. From degrees 80 through 300, over 98% of the gravitational signature is associated with topography, a result that reflects the preservation of crater relief in highly fractured crust. The remaining 2% represents fine details of subsurface structure not previously resolved. GRAIL elucidates the role of impact bombardment in homogenizing the distribution of shallow density anomalies on terrestrial planetary bodies.
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Affiliation(s)
- Maria T Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139-4307, USA.
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14
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Nerem RS, Jekeli C, Kaula WM. Gravity field determination and characteristics: Retrospective and prospective. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/94jb03257] [Citation(s) in RCA: 40] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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15
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Zuber MT, Smith DE, Phillips RJ, Solomon SC, Neumann GA, Hauck SA, Peale SJ, Barnouin OS, Head JW, Johnson CL, Lemoine FG, Mazarico E, Sun X, Torrence MH, Freed AM, Klimczak C, Margot JL, Oberst J, Perry ME, McNutt RL, Balcerski JA, Michel N, Talpe MJ, Yang D. Topography of the Northern Hemisphere of Mercury from MESSENGER Laser Altimetry. Science 2012; 336:217-20. [DOI: 10.1126/science.1218805] [Citation(s) in RCA: 144] [Impact Index Per Article: 12.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Affiliation(s)
- Maria T. Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - David E. Smith
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Roger J. Phillips
- Planetary Science Directorate, Southwest Research Institute, Boulder, CO 80302, USA
| | - Sean C. Solomon
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | | | - Steven A. Hauck
- Department of Earth, Environmental and Planetary Sciences, Case Western Reserve University, Cleveland, OH 44106, USA
| | - Stanton J. Peale
- Department of Physics, University of California, Santa Barbara, CA 93106, USA
| | | | - James W. Head
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA
| | - Catherine L. Johnson
- Department of Earth and Ocean Sciences, University of British Columbia, Vancouver, BC V6T 1Z4, Canada
| | | | - Erwan Mazarico
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Xiaoli Sun
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - Mark H. Torrence
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
- Stinger Ghaffarian Technologies Inc., 7701 Greenbelt Road, Greenbelt, MD 20770, USA
| | - Andrew M. Freed
- Department of Earth and Atmospheric Sciences, Purdue University, West Lafayette, IN 47907, USA
| | - Christian Klimczak
- Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA
| | - Jean-Luc Margot
- Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095, USA
| | - Jürgen Oberst
- Institute of Planetary Research, German Aerospace Center, Berlin D-12489, Germany
| | - Mark E. Perry
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - Ralph L. McNutt
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
| | - Jeffrey A. Balcerski
- Department of Earth, Environmental and Planetary Sciences, Case Western Reserve University, Cleveland, OH 44106, USA
| | - Nathalie Michel
- Department of Earth, Environmental and Planetary Sciences, Case Western Reserve University, Cleveland, OH 44106, USA
| | - Matthieu J. Talpe
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Di Yang
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
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Scholten F, Oberst J, Matz KD, Roatsch T, Wählisch M, Speyerer EJ, Robinson MS. GLD100: The near-global lunar 100 m raster DTM from LROC WAC stereo image data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003926] [Citation(s) in RCA: 152] [Impact Index Per Article: 12.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Jutzi M, Asphaug E. Forming the lunar farside highlands by accretion of a companion moon. Nature 2011; 476:69-72. [PMID: 21814278 DOI: 10.1038/nature10289] [Citation(s) in RCA: 59] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/08/2011] [Accepted: 06/13/2011] [Indexed: 11/09/2022]
Abstract
The most striking geological feature of the Moon is the terrain and elevation dichotomy between the hemispheres: the nearside is low and flat, dominated by volcanic maria, whereas the farside is mountainous and deeply cratered. Associated with this geological dichotomy is a compositional and thermal variation, with the nearside Procellarum KREEP (potassium/rare-earth element/phosphorus) Terrane and environs interpreted as having thin, compositionally evolved crust in comparison with the massive feldspathic highlands. The lunar dichotomy may have been caused by internal effects (for example spatial variations in tidal heating, asymmetric convective processes or asymmetric crystallization of the magma ocean) or external effects (such as the event that formed the South Pole/Aitken basin or asymmetric cratering). Here we consider its origin as a late carapace added by the accretion of a companion moon. Companion moons are a common outcome of simulations of Moon formation from a protolunar disk resulting from a giant impact, and although most coplanar configurations are unstable, a ∼1,200-km-diameter moon located at one of the Trojan points could be dynamically stable for tens of millions of years after the giant impact. Most of the Moon's magma ocean would solidify on this timescale, whereas the companion moon would evolve more quickly into a crust and a solid mantle derived from similar disk material, and would presumably have little or no core. Its likely fate would be to collide with the Moon at ∼2-3 km s(-1), well below the speed of sound in silicates. According to our simulations, a large moon/Moon size ratio (∼0.3) and a subsonic impact velocity lead to an accretionary pile rather than a crater, contributing a hemispheric layer of extent and thickness consistent with the dimensions of the farside highlands and in agreement with the degree-two crustal thickness profile. The collision furthermore displaces the KREEP-rich layer to the opposite hemisphere, explaining the observed concentration.
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Affiliation(s)
- M Jutzi
- Earth and Planetary Sciences Department, University of California, Santa Cruz, 1156 Highstreet, Santa Cruz, California 95060, USA.
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Zuber MT. Making mountains out of a moon. Nature 2011; 476:36-7. [DOI: 10.1038/476036a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Hagerty JJ, Lawrence DJ, Hawke BR. Thorium abundances of basalt ponds in South Pole-Aitken basin: Insights into the composition and evolution of the far side lunar mantle. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003723] [Citation(s) in RCA: 13] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Garrick-Bethell I, Nimmo F, Wieczorek MA. Structure and formation of the lunar farside highlands. Science 2010; 330:949-51. [PMID: 21071665 DOI: 10.1126/science.1193424] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The formation of the lunar farside highlands has long been an open problem in lunar science. We show that much of the topography and crustal thickness in this terrain can be described by a degree-2 harmonic. No other portion of the Moon exhibits comparable degree-2 structure. The quantified structure of the farside highlands unites them with the nearside and suggests a relation between lunar crustal structure, nearside volcanism, and heat-producing elements. The farside topography cannot be explained by a frozen-in tidal bulge. However, the farside crustal thickness and the topography it produces may have been caused by spatial variations in tidal heating when the ancient crust was decoupled from the mantle by a liquid magma ocean, similar to Europa's present ice shell.
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Affiliation(s)
- Ian Garrick-Bethell
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA.
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Nozette S, Rustan P, Pleasance LP, Kordas JF, Lewis IT, Park HS, Priest RE, Horan DM, Regeon P, Lichtenberg CL, Shoemaker EM, Eliason EM, McEwen AS, Robinson MS, Spudis PD, Acton CH, Buratti BJ, Duxbury TC, Baker DN, Jakosky BM, Blamont JE, Corson MP, Resnick JH, Rollins CJ, Davies ME, Lucey PG, Malaret E, Massie MA, Pieters CM, Reisse RA, Simpson RA, Smith DE, Sorenson TC, Breugge RW, Zuber MT. The clementine mission to the moon: scientific overview. Science 2010; 266:1835-9. [PMID: 17737076 DOI: 10.1126/science.266.5192.1835] [Citation(s) in RCA: 293] [Impact Index Per Article: 20.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
In the course of 71 days in lunar orbit, from 19 February to 3 May 1994, the Clementine spacecraft acquired just under two million digital images of the moon at visible and infrared wavelengths. These data are enabling the global mapping of the rock types of the lunar crust and the first detailed investigation of the geology of the lunar polar regions and the lunar far side. In addition, laser-ranging measurements provided the first view of the global topographic figure of the moon. The topography of many ancient impact basins has been measured, and a global map of the thickness of the lunar crust has been derived from the topography and gravity.
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Ping J, Huang Q, Su X, Tang G, Shu R, Xiao L, Huang J. Chang’E-1 orbiter discovers a lunar nearside volcano: YUTU Mountain. Sci Bull (Beijing) 2009. [DOI: 10.1007/s11434-009-0671-8] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
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Araki H, Tazawa S, Noda H, Ishihara Y, Goossens S, Sasaki S, Kawano N, Kamiya I, Otake H, Oberst J, Shum C. Lunar Global Shape and Polar Topography Derived from Kaguya-LALT Laser Altimetry. Science 2009; 323:897-900. [DOI: 10.1126/science.1164146] [Citation(s) in RCA: 216] [Impact Index Per Article: 14.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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Namiki N, Iwata T, Matsumoto K, Hanada H, Noda H, Goossens S, Ogawa M, Kawano N, Asari K, Tsuruta SI, Ishihara Y, Liu Q, Kikuchi F, Ishikawa T, Sasaki S, Aoshima C, Kurosawa K, Sugita S, Takano T. Farside Gravity Field of the Moon from Four-Way Doppler Measurements of SELENE (Kaguya). Science 2009; 323:900-5. [DOI: 10.1126/science.1168029] [Citation(s) in RCA: 148] [Impact Index Per Article: 9.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Noriyuki Namiki
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Takahiro Iwata
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Koji Matsumoto
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Hideo Hanada
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Hirotomo Noda
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Sander Goossens
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Mina Ogawa
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Nobuyuki Kawano
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Kazuyoshi Asari
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Sei-itsu Tsuruta
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Yoshiaki Ishihara
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Qinghui Liu
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Fuyuhiko Kikuchi
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Toshiaki Ishikawa
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Sho Sasaki
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Chiaki Aoshima
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Kosuke Kurosawa
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Seiji Sugita
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
| | - Tadashi Takano
- Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
- National Astronomical Observatory of Japan, 2-12 Hoshigaoka, Mizusawa, Oshu, Iwate 023-0861, Japan
- Japan Aerospace Exploration Agency, Tsukuba Space Center, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- Fujitsu Ltd., 1-9-3 Nakase, Mihama-ku, Chiba 261-8588, Japan
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Smrekar SE. Geologic evolution of the Martian dichotomy in the Ismenius area of Mars and implications for plains magnetization. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002260] [Citation(s) in RCA: 18] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Chevrel SD, Pinet PC, Daydou Y, Maurice S, Lawrence DJ, Feldman WC, Lucey PG. Integration of the Clementine UV-VIS spectral reflectance data and the Lunar Prospector gamma-ray spectrometer data: A global-scale multielement analysis of the lunar surface using iron, titanium, and thorium abundances. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2000je001419] [Citation(s) in RCA: 26] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- S. D. Chevrel
- Groupe de Recherches de Géodésie Spatiale; Observatoire Midi-Pyrénées; Toulouse France
| | - P. C. Pinet
- Groupe de Recherches de Géodésie Spatiale; Observatoire Midi-Pyrénées; Toulouse France
| | - Y. Daydou
- Groupe de Recherches de Géodésie Spatiale; Observatoire Midi-Pyrénées; Toulouse France
| | - S. Maurice
- Observatoire Midi-Pyrénées; Toulouse France
| | - D. J. Lawrence
- Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - W. C. Feldman
- Los Alamos National Laboratory; Los Alamos New Mexico USA
| | - P. G. Lucey
- Hawaii Institute of Geophysics and Planetology; University of Hawaii; Honolulu Hawaii USA
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Pieters CM, Head JW, Gaddis L, Jolliff B, Duke M. Rock types of South Pole-Aitken basin and extent of basaltic volcanism. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001414] [Citation(s) in RCA: 144] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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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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Freed AM, Melosh HJ, Solomon SC. Tectonics of mascon loading: Resolution of the strike-slip faulting paradox. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001347] [Citation(s) in RCA: 58] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Abstract
Clues to the history of Mars are recorded in the chemistry and structure of the planet's crust and mantle. The mantle is the rocky, interior region of the planet that transports heat generated during accretion and subsequent core formation. The crust formed by melting of the upper mantle, and has been shaped and re-distributed by impact, volcanism, mantle flow and erosion. Observations point to a dynamically active interior in the early phases of martian history, followed by a rapid fall-off in heat transport that significantly influenced the geological, geophysical and geochemical evolution of the planet, including the history of water and climate.
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Affiliation(s)
- M T Zuber
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139-4307, USA.
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Hiesinger H, Jaumann R, Neukum G, Head JW. Ages of mare basalts on the lunar nearside. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/2000je001244] [Citation(s) in RCA: 270] [Impact Index Per Article: 11.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Wieczorek MA, Phillips RJ. The “Procellarum KREEP Terrane”: Implications for mare volcanism and lunar evolution. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001092] [Citation(s) in RCA: 235] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Craddock RA, Howard AD. Simulated degradation of lunar impact craters and a new method for age dating farside mare deposits. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001099] [Citation(s) in RCA: 66] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cook AC, Watters TR, Robinson MS, Spudis PD, Bussey DBJ. Lunar polar topography derived from Clementine stereoimages. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001083] [Citation(s) in RCA: 30] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Zuber MT, Solomon SC, Phillips RJ, Smith DE, Tyler GL, Aharonson O, Balmino G, Banerdt WB, Head JW, Johnson CL, Lemoine FG, McGovern PJ, Neumann GA, Rowlands DD, Zhong S. Internal structure and early thermal evolution of Mars from Mars Global Surveyor topography and gravity. Science 2000; 287:1788-93. [PMID: 10710301 DOI: 10.1126/science.287.5459.1788] [Citation(s) in RCA: 457] [Impact Index Per Article: 19.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Topography and gravity measured by the Mars Global Surveyor have enabled determination of the global crust and upper mantle structure of Mars. The planet displays two distinct crustal zones that do not correlate globally with the geologic dichotomy: a region of crust that thins progressively from south to north and encompasses much of the southern highlands and Tharsis province and a region of approximately uniform crustal thickness that includes the northern lowlands and Arabia Terra. The strength of the lithosphere beneath the ancient southern highlands suggests that the northern hemisphere was a locus of high heat flow early in martian history. The thickness of the elastic lithosphere increases with time of loading in the northern plains and Tharsis. The northern lowlands contain structures interpreted as large buried channels that are consistent with northward transport of water and sediment to the lowlands before the end of northern hemisphere resurfacing.
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Affiliation(s)
- M T Zuber
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA.
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Jolliff BL, Gillis JJ, Haskin LA, Korotev RL, Wieczorek MA. Major lunar crustal terranes: Surface expressions and crust-mantle origins. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001103] [Citation(s) in RCA: 585] [Impact Index Per Article: 24.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Zhong S, Zuber MT. Long-wavelength topographic relaxation for self-gravitating planets and implications for the time-dependent compensation of surface topography. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001075] [Citation(s) in RCA: 67] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Bussey DBJ, Spudis PD. Compositional studies of the Orientale, Humorum, Nectaris, and Crisium lunar basins. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001130] [Citation(s) in RCA: 39] [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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Smith DE, Sjogren WL, Tyler GL, Balmino G, Lemoine FG, Konopliv AS. The gravity field of Mars: results from Mars Global Surveyor. Science 1999; 286:94-7. [PMID: 10506567 DOI: 10.1126/science.286.5437.94] [Citation(s) in RCA: 113] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Observations of the gravity field of Mars reveal a planet that has responded differently in its northern and southern hemispheres to major impacts and volcanic processes. The rough, elevated southern hemisphere has a relatively featureless gravitational signature indicating a state of near-isostatic compensation, whereas the smooth, low northern plains display a wider range of gravitational anomalies that indicates a thinner but stronger surface layer than in the south. The northern hemisphere shows evidence for buried impact basins, although none large enough to explain the hemispheric elevation difference. The gravitational potential signature of Tharsis is approximately axisymmetric and contains the Tharsis Montes but not the Olympus Mons or Alba Patera volcanoes. The gravity signature of Valles Marineris extends into Chryse and provides an estimate of material removed by early fluvial activity.
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Affiliation(s)
- D E Smith
- Laboratory for Terrestrial Physics, National Aeronautics and Space Administration (NASA) Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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Pieters CM, Tompkins S. Tsiolkovsky crater: A window into crustal processes on the lunar farside. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1998je001010] [Citation(s) in RCA: 44] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Yingst RA, Head JW. Geology of mare deposits in South Pole-Aitken basin as seen by Clementine UV/VIS data. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1999je900016] [Citation(s) in RCA: 33] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Smith DE, Zuber MT, Solomon SC, Phillips RJ, Head JW, Garvin JB, Banerdt WB, Muhleman DO, Pettengill GH, Neumann GA, Lemoine FG, Abshire JB, Aharonson O, Brown CD, Hauck SA, Ivanov AB, McGovern PJ, Zwally HJ, Duxbury TC. The global topography of Mars and implications for surface evolution. Science 1999; 284:1495-503. [PMID: 10348732 DOI: 10.1126/science.284.5419.1495] [Citation(s) in RCA: 714] [Impact Index Per Article: 28.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Elevations measured by the Mars Orbiter Laser Altimeter have yielded a high-accuracy global map of the topography of Mars. Dominant features include the low northern hemisphere, the Tharsis province, and the Hellas impact basin. The northern hemisphere depression is primarily a long-wavelength effect that has been shaped by an internal mechanism. The topography of Tharsis consists of two broad rises. Material excavated from Hellas contributes to the high elevation of the southern hemisphere and to the scarp along the hemispheric boundary. The present topography has three major drainage centers, with the northern lowlands being the largest. The two polar cap volumes yield an upper limit of the present surface water inventory of 3.2 to 4.7 million cubic kilometers.
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Affiliation(s)
- D E Smith
- Earth Sciences Directorate, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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Konopliv AS, Binder AB, Hood LL, Kucinskas AB, Sjogren WL, Williams JG. Improved gravity field of the moon from lunar prospector. Science 1998; 281:1476-80. [PMID: 9727968 DOI: 10.1126/science.281.5382.1476] [Citation(s) in RCA: 208] [Impact Index Per Article: 8.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
An improved gravity model from Doppler tracking of the Lunar Prospector (LP) spacecraft reveals three new large mass concentrations (mascons) on the nearside of the moon beneath the impact basins Mare Humboltianum, Mendel-Ryberg, and Schiller-Zucchius, where the latter basin has no visible mare fill. Although there is no direct measurement of the lunar farside gravity, LP partially resolves four mascons in the large farside basins of Hertzsprung, Coulomb-Sarton, Freundlich-Sharonov, and Mare Moscoviense. The center of each of these basins contains a gravity maximum relative to the surrounding basin. The improved normalized polar moment of inertia (0.3932 +/- 0.0002) is consistent with an iron core with a radius of 220 to 450 kilometers.
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Affiliation(s)
- AS Konopliv
- A. S. Konopliv, A. B. Kucinskas, W. L. Sjogren, J. G. Williams, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. A. B. Binder, Lunar Research Institute, Gilroy, CA 95020, USA. L. L. Hood, University of Arizona
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Lucey PG, Taylor GJ, Hawke BR, Spudis PD. FeO and TiO2concentrations in the South Pole-Aitken basin: Implications for mantle composition and basin formation. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/97je03146] [Citation(s) in RCA: 100] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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