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Zhang F, Pizzi A, Ruj T, Komatsu G, Yin A, Dang Y, Liu Y, Zou Y. Evidence for structural control of mare volcanism in lunar compressional tectonic settings. Nat Commun 2023; 14:2892. [PMID: 37210379 DOI: 10.1038/s41467-023-38615-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/04/2022] [Accepted: 05/08/2023] [Indexed: 05/22/2023] Open
Abstract
One of the long-standing enigmas for lunar tectonic-thermal evolution is the spatiotemporal association of contractional wrinkle ridges and basaltic volcanism in a compressional regime. Here, we show that most of the 30 investigated volcanic (eruptive) centers are linked to contractional wrinkle ridges developed above preexisting basin basement-involved ring/rim normal faults. Based on the tectonic patterns associated with the basin formation and mass loading and considering that during the subsequent compression the stress was not purely isotropic, we hypothesize that tectonic inversion produced not only thrust faults but also reactivated structures with strike-slip and even extensional components, thus providing a valid mechanism for magma transport through fault planes during ridge faulting and folding of basaltic layers. Our findings suggest that lunar syn-tectonic mare emplacement along reactivated inherited faults provides important records of basin-scale structure-involved volcanism, which is more complex than previously considered.
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Affiliation(s)
- Feng Zhang
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, China.
| | - Alberto Pizzi
- Department of Engineering and Geology, Università d'Annunzio, Chieti-Pescara, Italy.
| | - Trishit Ruj
- Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Sagamihara, Kanagawa, 252-5210, Japan
| | - Goro Komatsu
- Department of Engineering and Geology, Università d'Annunzio, Chieti-Pescara, Italy
- International Research School of Planetary Sciences, Università d'Annunzio, Pescara, Italy
| | - An Yin
- Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles, CA, 90095-1567, USA
| | - Yanan Dang
- National Key Laboratory of Microwave Imaging Technology, Aerospace Information Research Institute, Chinese Academy of Sciences, Bejing, China
| | - Yang Liu
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, China
- Center for Excellence in Comparative Planetology, Chinese Academy of Sciences, Hefei, 200083, China
| | - Yongliao Zou
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, China
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Recognition of Sedimentary Rock Occurrences in Satellite and Aerial Images of Other Worlds—Insights from Mars. REMOTE SENSING 2021. [DOI: 10.3390/rs13214296] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/31/2022]
Abstract
Sedimentary rocks provide records of past surface and subsurface processes and environments. The first step in the study of the sedimentary rock record of another world is to learn to recognize their occurrences in images from instruments aboard orbiting, flyby, or aerial platforms. For two decades, Mars has been known to have sedimentary rocks; however, planet-wide identification is incomplete. Global coverage at 0.25–6 m/pixel, and observations from the Curiosity rover in Gale crater, expand the ability to recognize Martian sedimentary rocks. No longer limited to cases that are light-toned, lightly cratered, and stratified—or mimic original depositional setting (e.g., lithified deltas)—Martian sedimentary rocks include dark-toned examples, as well as rocks that are erosion-resistant enough to retain small craters as well as do lava flows. Breakdown of conglomerates, breccias, and even some mudstones, can produce a pebbly regolith that imparts a “smooth” appearance in satellite and aerial images. Context is important; sedimentary rocks remain challenging to distinguish from primary igneous rocks in some cases. Detection of ultramafic, mafic, or andesitic compositions do not dictate that a rock is igneous, and clast genesis should be considered separately from the depositional record. Mars likely has much more sedimentary rock than previously recognized.
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Watters TR, James PB, Selvans MM. Mercury's Crustal Thickness and Contractional Strain. GEOPHYSICAL RESEARCH LETTERS 2021; 48:e2021GL093528. [PMID: 35860428 PMCID: PMC9285554 DOI: 10.1029/2021gl093528] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/24/2021] [Revised: 07/12/2021] [Accepted: 07/16/2021] [Indexed: 06/15/2023]
Abstract
The crust of Mercury has experienced contraction on a global scale. Contractional deformation is expressed by a broadly distributed network of lobate thrust fault scarps. The most likely principal source of stress is global contraction from cooling of Mercury's interior. Global contraction alone would be expected to result in a uniformly distributed population of thrust faults. Mercury's fault scarps, however, often occur in long, linear clusters or bands. An analysis of the contractional strain as a function of crustal thickness, estimated in two crustal thickness models (CT1 and CT2) derived from gravity and topography data obtained during the MESSENGER mission, indicates the greatest contractional strain occurs in crust 50-60 km thick. On Earth, mantle downwelling can thicken and compress overlying crust, regionally concentrating thrust faults. Clusters of lobate scarps collocated with regions of thick crust suggest downward mantle flow contributed to the localization of lithosphere-penetrating thrust faults.
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Affiliation(s)
- Thomas R. Watters
- Center for Earth and Planetary StudiesNational Air and Space MuseumSmithsonian InstitutionWashingtonDCUSA
| | | | - Michelle M. Selvans
- Center for Earth and Planetary StudiesNational Air and Space MuseumSmithsonian InstitutionWashingtonDCUSA
- Geology DepartmentClovis Community CollegeFresnoCAUSA
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Watters TR. A case for limited global contraction of Mercury. COMMUNICATIONS EARTH & ENVIRONMENT 2021; 2:9. [PMID: 33490970 PMCID: PMC7808997 DOI: 10.1038/s43247-020-00076-5] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/20/2020] [Accepted: 11/24/2020] [Indexed: 06/12/2023]
Abstract
Mercury is a one-plate planet that has experienced significant radial contraction primarily driven by interior cooling. In some previous studies aimed at estimating the total magnitude of contraction, numerous faults are assigned to positive relief landforms, many without evidence of origin by deformation, resulting in estimates of planetary radius reduction as large as 7 km. Here we use high-incidence angle image mosaics and topography from the MESSENGER mission to map Mercury's contractional landforms. Each landform is assigned a single, principal fault, resulting in an amount of contractional strain equivalent to a radius change of no more than 1 to 2 km. A small radius change since the end of heavy bombardment is consistent with Mercury's long-lived magnetic field and evidence of recent tectonic activity. It is concluded that the retention of interior heat and a lower degree of contraction may be facilitated by the insulating effect of a thick megaregolith.
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Affiliation(s)
- Thomas R. Watters
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560-0315 USA
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An Integrated Geologic Map of the Rembrandt Basin, on Mercury, as a Starting Point for Stratigraphic Analysis. REMOTE SENSING 2020. [DOI: 10.3390/rs12193213] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
Planetary geologic maps are usually carried out following a morpho-stratigraphic approach where morphology is the dominant character guiding the remote sensing image interpretation. On the other hand, on Earth a more comprehensive stratigraphic approach is preferred, using lithology, overlapping relationship, genetic source, and ages as the main discriminants among the different geologic units. In this work we produced two different geologic maps of the Rembrandt basin of Mercury, following the morpho-stratigraphic methods and symbology adopted by many authors while mapping quadrangles on Mercury, and an integrated geo-stratigraphic approach, where geologic units were distinguished also on the basis of their false colors (derived by multispectral image data of the NASA MESSENGER mission), subsurface stratigraphic position (inferred by crater excavation) and model ages. We distinguished two different resurfacing events within the Rembrandt basin, after the impact event, and four other smooth plains units outside the basin itself. This provided the basis to estimate thicknesses, volumes, and ages of the smooth plains inside the basin. Results from thickness estimates obtained using different methodologies confirm the presence of two distinct volcanic events inside the Rembrandt basin, with a total thickness ranging between 1–1.5 km. Furthermore, model ages suggest that the volcanic infilling of the Rembrandt basin is among the ones that extended well into the mid-Calorian period, when Mercury’s effusive volcanism was previously thought to be largely over.
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López I, Hansen VL. Geologic Map of the Niobe Planitia Region (I-2467), Venus. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2020; 7:e2020EA001171. [PMID: 33134436 PMCID: PMC7583383 DOI: 10.1029/2020ea001171] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 03/12/2020] [Revised: 06/09/2020] [Accepted: 06/16/2020] [Indexed: 06/11/2023]
Abstract
We present a 1:10M scale geologic map of the Niobe Planitia region of Venus (0°N-57°N/60°E-180°E). We herein refer to this area as the Niobe Map Area (NMA). Geologic mapping employed NASA Magellan synthetic aperture radar and altimetry data. The NMA geologic map and its companion Aphrodite Map Area (AMA) cover ~25% of Venus' surface, providing an important and unique perspective to study global and regional geologic processes. Both areas display a regional coherence of preserved geologic patterns that record three sequential geologic eras: the ancient era, the Artemis superstructure era, and the youngest fracture zone era. The NMA preserves a limited record of the fracture zone era, contrary to the AMA. However, the NMA hosts a diverse and rich assemblage of material and structures of the ancient era and structures that define the Artemis superstructure era. These two eras likely overlap in time and account for the formation of basement materials and lower plain units. Impact craters formed throughout the NMA recorded history. Approximately 40% of the impact craters show interior flood deposits, indicating that a significant number of NMA impact craters experienced notable geological events after impact crater formation. This and other geologic relations record a geohistory inconsistent with postulated global catastrophic resurfacing. Together, the NMA and the AMA record a rich geologic history of the surface of Venus that provide a framework to formulate new working hypotheses of Venus evolution and to plan future studies of the planet.
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Affiliation(s)
- Iván López
- Departamento de Biología y Geología, Física y Química InorgánicaUniversidad Rey Juan CarlosMadridSpain
| | - Vicki L. Hansen
- Department of Earth and Environmental SciencesUniversity of Minnesota‐DuluthDuluthMNUSA
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Cole HM, Andrews-Hanna JC. The anatomy of a wrinkle ridge revealed in the wall of Melas Chasma, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2017; 122:889-900. [PMID: 31534880 PMCID: PMC6750226 DOI: 10.1002/2017je005274] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Wrinkle ridges are among the most common tectonic structures on the terrestrial planets, and provide important records of the history of planetary strain and geodynamics. The observed broad arches and superposed narrow wrinkles are thought to be the surface manifestation of blind thrust faults, which terminate in near-surface volcanic sequences and cause folding and layer-parallel shear. However, the subsurface tectonic architecture associated with the ridges remains a matter of debate. Here we present direct observations of a wrinkle ridge thrust fault where it has been exposed by erosion in the southern wall of Melas Chasma on Mars. The thrust fault has been made resistant to erosion, likely due to volcanic intrusion, such that later erosional widening of the trough exposed the fault plane as a 70 km-long ridge extending into the chasma. A plane fit to this ridge crest reveals a thrust fault with a dip of 13° (+8°, -7°) between 1 and 3.5 km depth below the plateau surface, with no evidence for listric character in this depth range. This dip is significantly lower than the commonly assumed value of 30°, which, if representative of other wrinkle ridges, indicates that global contraction on Mars may have been previously underestimated.
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Affiliation(s)
- Hank M. Cole
- Department of Geophysics, Colorado School of Mines, Golden CO 80401
| | - Jeffrey C. Andrews-Hanna
- Southwest Research Institute, Boulder, CO 80302
- now at the Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0092
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8
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Watters TR. Origin of periodically spaced wrinkle ridges on the Tharsis Plateau of Mars. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/91je01402] [Citation(s) in RCA: 94] [Impact Index Per Article: 7.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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9
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Tanaka KL, Golombek MP, Banerdt WB. Reconciliation of stress and structural histories of the Tharsis region of Mars. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/91je01194] [Citation(s) in RCA: 159] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Banks ME, Watters TR, Robinson MS, Tornabene LL, Tran T, Ojha L, Williams NR. Morphometric analysis of small-scale lobate scarps on the Moon using data from the Lunar Reconnaissance Orbiter. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003907] [Citation(s) in RCA: 36] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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11
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Watters TR, Robinson MS, Beyer RA, Banks ME, Bell JF, Pritchard ME, Hiesinger H, van der Bogert CH, Thomas PC, Turtle EP, Williams NR. Evidence of Recent Thrust Faulting on the Moon Revealed by the Lunar Reconnaissance Orbiter Camera. Science 2010; 329:936-40. [PMID: 20724632 DOI: 10.1126/science.1189590] [Citation(s) in RCA: 102] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Thomas R. Watters
- Center for Earth and Planetary Studies, Smithsonian Institution, Washington, DC 20560, USA
| | - Mark S. Robinson
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85251, USA
| | - Ross A. Beyer
- Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA
- NASA Ames Research Center, Moffett Field, CA 94035–0001, USA
| | - Maria E. Banks
- Center for Earth and Planetary Studies, Smithsonian Institution, Washington, DC 20560, USA
| | - James F. Bell
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
| | - Matthew E. Pritchard
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY 14853, USA
| | - Harald Hiesinger
- Institut für Planetologie, Westfälische Wilhelms-Universität, 48149 Münster, Germany
- Department of Geological Sciences, Brown University, Box 1846, Providence, RI 02912, USA
| | | | - Peter C. Thomas
- Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
| | | | - Nathan R. Williams
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY 14853, USA
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Ivanov MA, Korteniemi J, Kostama VP, Raitala J, Törmänen T, Neukum G. Major episodes in the geologic history of western Promethei Terra, Mars. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2008je003256] [Citation(s) in RCA: 11] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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13
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Leverington DW. Reconciling channel formation processes with the nature of elevated outflow systems at Ophir and Aurorae Plana, Mars. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003398] [Citation(s) in RCA: 27] [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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14
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Watters TR, Head JW, Solomon SC, Robinson MS, Chapman CR, Denevi BW, Fassett CI, Murchie SL, Strom RG. Evolution of the Rembrandt impact basin on Mercury. Science 2009; 324:618-21. [PMID: 19407197 DOI: 10.1126/science.1172109] [Citation(s) in RCA: 38] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
MESSENGER's second Mercury flyby revealed a ~715-kilometer-diameter impact basin, the second-largest well-preserved basin-scale impact structure known on the planet. The Rembrandt basin is comparable in age to the Caloris basin, is partially flooded by volcanic plains, and displays a unique wheel-and-spoke-like pattern of basin-radial and basin-concentric wrinkle ridges and graben. Stratigraphic relations indicate a multistaged infilling and deformational history involving successive or overlapping phases of contractional and extensional deformation. The youngest deformation of the basin involved the formation of a approximately 1000-kilometer-long lobate scarp, a product of the global cooling and contraction of Mercury.
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Affiliation(s)
- Thomas R Watters
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA.
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15
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Fergason RL, Christensen PR. Formation and erosion of layered materials: Geologic and dust cycle history of eastern Arabia Terra, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002973] [Citation(s) in RCA: 24] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Murchie SL, Watters TR, Robinson MS, Head JW, Strom RG, Chapman CR, Solomon SC, McClintock WE, Prockter LM, Domingue DL, Blewett DT. Geology of the Caloris Basin, Mercury: A View from MESSENGER. Science 2008; 321:73-6. [DOI: 10.1126/science.1159261] [Citation(s) in RCA: 119] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Scott L. Murchie
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Thomas R. Watters
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Mark S. Robinson
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - James W. Head
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Robert G. Strom
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Clark R. Chapman
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Sean C. Solomon
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - William E. McClintock
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Louise M. Prockter
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - Deborah L. Domingue
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
| | - David T. Blewett
- Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20015, USA
- Department of Geological Sciences, Arizona State University, Tempe, AZ 85251, USA
- Department of Geological Sciences, Brown University, Providence, RI 02906, USA
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA
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Basilevsky AT, Head JW. Impact craters on regional plains on Venus: Age relations with wrinkle ridges and implications for the geological evolution of Venus. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002473] [Citation(s) in RCA: 25] [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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Bondarenko NV, Kreslavsky MA, Head JW. North-south roughness anisotropy on Venus from the Magellan Radar Altimeter: Correlation with geology. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002599] [Citation(s) in RCA: 14] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Martínez-Alonso S. A volcanic interpretation of Gusev Crater surface materials from thermophysical, spectral, and morphological evidence. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002327] [Citation(s) in RCA: 49] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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21
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Leverington DW. An igneous origin for features of a candidate crater-lake system in western Memnonia, Mars. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002237] [Citation(s) in RCA: 47] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Montési LGJ. Clues to the lithospheric structure of Mars from wrinkle ridge sets and localization instability. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je001974] [Citation(s) in RCA: 82] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Affiliation(s)
- Robert A. Craddock
- Center for Earth and Planetary Studies, National Air and Space Museum; Smithsonian Institution; Washington District of Columbia USA
| | - Alan D. Howard
- Department of Environmental Sciences; University of Virginia; Charlottesville Virginia USA
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Head JW. Northern lowlands of Mars: Evidence for widespread volcanic flooding and tectonic deformation in the Hesperian Period. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2000je001445] [Citation(s) in RCA: 204] [Impact Index Per Article: 9.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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Golombek MP, Anderson FS, Zuber MT. Martian wrinkle ridge topography: Evidence for subsurface faults from MOLA. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001308] [Citation(s) in RCA: 121] [Impact Index Per Article: 5.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Anderson RC, Dohm JM, Golombek MP, Haldemann AFC, Franklin BJ, Tanaka KL, Lias J, Peer B. Primary centers and secondary concentrations of tectonic activity through time in the western hemisphere of Mars. ACTA ACUST UNITED AC 2001. [DOI: 10.1029/2000je001278] [Citation(s) in RCA: 262] [Impact Index Per Article: 11.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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27
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Schultz RA. Localization of bedding plane slip and backthrust faults above blind thrust faults: Keys to wrinkle ridge structure. ACTA ACUST UNITED AC 2000. [DOI: 10.1029/1999je001212] [Citation(s) in RCA: 147] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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28
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Kreslavsky MA, Basilevsky AT. Morphometry of wrinkle ridges on Venus: Comparison with other planets. ACTA ACUST UNITED AC 1998. [DOI: 10.1029/98je00360] [Citation(s) in RCA: 21] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Craddock RA, Crumpler LS, Aubele JC, Zimbelman JR. Geology of central Chryse Planitia and the Viking 1 landing site: Implications for the Mars Pathfinder mission. ACTA ACUST UNITED AC 1997. [DOI: 10.1029/97je00058] [Citation(s) in RCA: 26] [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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Allemand P, Thomas PG. Localization of Martian ridges by impact craters: Mechanical and chronological implications. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je03081] [Citation(s) in RCA: 23] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Pappalardo RT, Greeley R. A review of the origins of subparallel ridges and troughs: Generalized morphological predictions from terrestrial models. ACTA ACUST UNITED AC 1995. [DOI: 10.1029/94je02638] [Citation(s) in RCA: 36] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Crumpler LS, Head JW, Aubele JC. Relation of Major Volcanic Center Concentration on Venus to Global Tectonic Patterns. Science 1993; 261:591-5. [PMID: 17758169 DOI: 10.1126/science.261.5121.591] [Citation(s) in RCA: 52] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Global analysis of NASA Magellan image data indicates that a major concentration of volcanic centers covering approximately 40 percent of the surface of Venus occurs between the Beta, Atla, and Themis regiones. Associated with this enhanced concentration are geological characteristics commonly interpreted as rifting and mantle upwelling. Interconnected low plains in an annulus around this concentration are characterized by crustal shortening and infrequent volcanic centers that may represent sites of mantle return flow and net down-welling. Together, these observations suggest the existence of relatively simple, largescale patterns of mantle circulation similar to those associated with concentrations of intraplate volcanism on Earth.
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Solomon SC, Smrekar SE, Bindschadler DL, Grimm RE, Kaula WM, McGill GE, Phillips RJ, Saunders RS, Schubert G, Squyres SW, Stofan ER. Venus tectonics: An overview of Magellan observations. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je01418] [Citation(s) in RCA: 231] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Zuber MT, Mouginis-Mark PJ. Caldera subsidence and magma chamber depth of the Olympus Mons volcano, Mars. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je01770] [Citation(s) in RCA: 45] [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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Squyres SW, Jankowski DG, Simons M, Solomon SC, Hager BH, McGill GE. Plains tectonism on Venus: The deformation belts of Lavinia Planitia. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je00481] [Citation(s) in RCA: 55] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Suppe J, Connors C. Critical taper wedge mechanics of fold-and-thrust belts on Venus: Initial results from Magellan. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je01164] [Citation(s) in RCA: 52] [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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Solomon SC, Head JW, Kaula WM, McKenzie D, Parsons B, Phillips RJ, Schubert G, Talwani M. Venus Tectonics: Initial Analysis from Magellan. Science 1991; 252:297-312. [PMID: 17769277 DOI: 10.1126/science.252.5003.297] [Citation(s) in RCA: 102] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Radar imaging and altimetry data from the Magellan mission have revealed a diversity of deformational features at a variety of spatial scales on the Venus surface. The plains record a superposition of different episodes of deformation and volcanism; strain is both areally distributed and concentrated into zones of extension and shortening. The common coherence of strain patterns over hundreds of kilometers implies that many features in the plains reflect a crustal response to mantle dynamic processes. Ridge belts and mountain belts represent successive degrees of lithospheric shortening and crustal thickening; the mountain belts also show widespread evidence for extension and collapse both during and following crustal compression. Venus displays two geometrical patterns of concentrated lithospheric extension: quasi-circular coronae and broad rises with linear rift zones; both are sites of significant volcanism. No long, large-offset strike-slip faults have been observed, although limited local horizontal shear is accommodated across many zones of crustal shortening. In general, tectonic features on Venus are unlike those in Earth's oceanic regions in that strain typically is distributed across broad zones that are one to a few hundred kilometers wide, and separated by stronger and less deformed blocks hundreds of kilometers in width, as in actively deforming continental regions on Earth.
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Schultz RA. Structural development of Coprates Chasma and Western Ophir Planum, Valles Marineris Rift, Mars. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/91je02556] [Citation(s) in RCA: 72] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Zuber MT, Aist LL. The shallow structure of the Martian lithosphere in the vicinity of the ridged plains. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14215] [Citation(s) in RCA: 36] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Craddock RA, Maxwell TA. Resurfacing of the Martian Highlands in the Amenthes and Tyrrhena region. ACTA ACUST UNITED AC 1990. [DOI: 10.1029/jb095ib09p14265] [Citation(s) in RCA: 61] [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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