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Rodriguez JAP, Leonard GJ, Kargel JS, Domingue D, Berman DC, Banks M, Zarroca M, Linares R, Marchi S, Baker VR, Webster KD, Sykes M. The Chaotic Terrains of Mercury Reveal a History of Planetary Volatile Retention and Loss in the Innermost Solar System. Sci Rep 2020; 10:4737. [PMID: 32179758 PMCID: PMC7075900 DOI: 10.1038/s41598-020-59885-5] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/11/2019] [Accepted: 01/24/2020] [Indexed: 11/25/2022] Open
Abstract
Mercury’s images obtained by the 1974 Mariner 10 flybys show extensive cratered landscapes degraded into vast knob fields, known as chaotic terrain (AKA hilly and lineated terrain). For nearly half a century, it was considered that these terrains formed due to catastrophic quakes and ejecta fallout produced by the antipodal Caloris basin impact. Here, we present the terrains’ first geologic examination based on higher spatial resolution MESSENGER (MErcury Surface Space ENvironment GEochemistry and Ranging) imagery and laser altimeter topography. Our surface age determinations indicate that their development persisted until ~1.8 Ga, or ~2 Gyrs after the Caloris basin formed. Furthermore, we identified multiple chaotic terrains with no antipodal impact basins; hence a new geological explanation is needed. Our examination of the Caloris basin’s antipodal chaotic terrain reveals multi-kilometer surface elevation losses and widespread landform retention, indicating an origin due to major, gradual collapse of a volatile-rich layer. Crater interior plains, possibly lavas, share the chaotic terrains’ age, suggesting a development associated with a geothermal disturbance above intrusive magma bodies, which best explains their regionality and the enormity of the apparent volume losses involved in their development. Furthermore, evidence of localized, surficial collapse, might reflect a complementary, and perhaps longer lasting, devolatilization history by solar heating.
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Affiliation(s)
- J Alexis P Rodriguez
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA.
| | - Gregory J Leonard
- Department of Planetary Sciences, University of Arizona, Tucson, AZ, USA
| | - Jeffrey S Kargel
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA
| | - Deborah Domingue
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA
| | - Daniel C Berman
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA
| | - Maria Banks
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA.,NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Mario Zarroca
- External Geodynamics and Hydrogeology Group, Department of Geology, Autonomous University of Barcelona, 08193, Bellaterra, Barcelona, Spain
| | - Rogelio Linares
- External Geodynamics and Hydrogeology Group, Department of Geology, Autonomous University of Barcelona, 08193, Bellaterra, Barcelona, Spain
| | - Simone Marchi
- Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO, USA
| | - Victor R Baker
- Department of Hydrology and Atmospheric Sciences, University of Arizona, Tucson, AZ, USA
| | - Kevin D Webster
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA
| | - Mark Sykes
- Planetary Science Institute, 1700 E Fort Lowell Road, Suite 106, Tucson, AZ, USA
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Fassett CI, Head JW, Baker DMH, Zuber MT, Smith DE, Neumann GA, Solomon SC, Klimczak C, Strom RG, Chapman CR, Prockter LM, Phillips RJ, Oberst J, Preusker F. Large impact basins on Mercury: Global distribution, characteristics, and modification history from MESSENGER orbital data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012je004154] [Citation(s) in RCA: 60] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Soha JM, Lynn DJ, Lorre JJ, Mosher JA, Thayer NN, Elliott DA, Benton WD, Dewar RE. IPL processing of the Mariner 10 images of Mercury. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb080i017p02394] [Citation(s) in RCA: 19] [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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Strom RG, Murray BC, Belton MJS, Danielson GE, Davies ME, Gault DE, Hapke B, O'Leary B, Trask N, Guest JE, Anderson J, Klaasen K. Preliminary imaging results from the second Mercury encounter. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/jb080i017p02345] [Citation(s) in RCA: 15] [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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Matsuyama I, Nimmo F. Gravity and tectonic patterns of Mercury: Effect of tidal deformation, spin-orbit resonance, nonzero eccentricity, despinning, and reorientation. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003252] [Citation(s) in RCA: 35] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Robinson MS, Lucey PG. Recalibrated Mariner 10 Color Mosaics: Implications for Mercurian Volcanism. Science 1997; 275:197-200. [PMID: 8985010 DOI: 10.1126/science.275.5297.197] [Citation(s) in RCA: 129] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/03/2023]
Abstract
Recalibration of Mariner 10 color image data allows the identification of distinct color units on the mercurian surface. We analyze these data in terms of opaque mineral abundance, iron content, and soil maturity and find color units consistent with the presence of volcanic deposits on Mercury's surface. Additionally, materials associated with some impact craters have been excavated from a layer interpreted to be deficient in opaque minerals within the crust, possibly analogous to the lunar anorthosite crust. These observations suggest that Mercury has undergone complex differentiation like the other terrestrial planets and the Earth's moon.
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Affiliation(s)
- MS Robinson
- M. S. Robinson, United States Geological Survey, 2255 North Gemini Drive, Flagstaff, Arizona, 86001, USA. P. G. Lucey, Hawaii Institute of Geophysics and Planetology, University of Hawaii, Honolulu, HI 96822, USA
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Abstract
The first unambiguous full-disk radar mapping of Mercury at 3.5-centimeter wavelength, with the Goldstone 70-meter antenna transmitting and 26 antennas of the Very Large Array receiving, has provided evidence for the presence of polar ice. The radar experiments, conducted on 8 and 23 August 1991, were designed to image the half of Mercury not photographed by Mariner 10. The orbital geometry allowed viewing beyond the north pole of Mercury; a highly reflective region was clearly visible on the north pole during both experiments. This polar region has areas in which the circular polarization ratio (pt) was 1.0 to 1.4; values < approximately 0.1 are typical for terrestrial planets. Such high values of have hitherto been observed in radar observations only from icy regions of Mars and icy outer planet satellites.
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