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Liu J, Qin X, Ren X, Wang X, Sun Y, Zeng X, Wu H, Chen Z, Chen W, Chen Y, Wang C, Sun Z, Zhang R, Ouyang Z, Guo Z, Head JW, Li C. Martian dunes indicative of wind regime shift in line with end of ice age. Nature 2023; 620:303-309. [PMID: 37407822 PMCID: PMC10412455 DOI: 10.1038/s41586-023-06206-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/02/2022] [Accepted: 05/12/2023] [Indexed: 07/07/2023]
Abstract
Orbital observations suggest that Mars underwent a recent 'ice age' (roughly 0.4-2.1 million years ago), during which a latitude-dependent ice-dust mantle (LDM)1,2 was emplaced. A subsequent decrease in obliquity amplitude resulted in the emergence of an 'interglacial period'1,3 during which the lowermost latitude LDM ice4-6 was etched and removed, returning it to the polar cap. These observations are consistent with polar cap stratigraphy1,7, but lower- to mid-latitude in situ surface observations in support of a glacial-interglacial transition that can be reconciled with mesoscale and global atmospheric circulation models8 is lacking. Here we present a suite of measurements obtained by the Zhurong rover during its traverse across the southern LDM region in Utopia Planitia, Mars. We find evidence for a stratigraphic sequence involving initial barchan dune formation, indicative of north-easterly winds, cementation of dune sediments, followed by their erosion by north-westerly winds, eroding the barchan dunes and producing distinctive longitudinal dunes, with the transition in wind regime consistent with the end of the ice age. The results are compatible with the Martian polar stratigraphic record and will help improve our understanding of the ancient climate history of Mars9.
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Affiliation(s)
- Jianjun Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Xiaoguang Qin
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Xin Ren
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Xu Wang
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Yong Sun
- State Key Laboratory of Tibetan Plateau Earth System, Resources and Environment, Institute of Tibetan Plateau Research, Chinese Academy of Sciences, Beijing, China
| | - Xingguo Zeng
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Haibin Wu
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Zhaopeng Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Wangli Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Yuan Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Cheng Wang
- Beijing Aerospace Control Center, Beijing, China
| | - Zezhou Sun
- Beijing Institute of Spacecraft System Engineering, Beijing, China
| | - Rongqiao Zhang
- Lunar Exploration and Space Engineering Center, Beijing, China
| | - Ziyuan Ouyang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, China
| | - Zhengtang Guo
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China.
| | - James W Head
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, RI, USA.
| | - Chunlai Li
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China.
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Newman CE, de la Torre Juárez M, Pla-García J, Wilson RJ, Lewis SR, Neary L, Kahre MA, Forget F, Spiga A, Richardson MI, Daerden F, Bertrand T, Viúdez-Moreiras D, Sullivan R, Sánchez-Lavega A, Chide B, Rodriguez-Manfredi JA. Multi-model Meteorological and Aeolian Predictions for Mars 2020 and the Jezero Crater Region. SPACE SCIENCE REVIEWS 2021; 217:20. [PMID: 33583960 PMCID: PMC7868679 DOI: 10.1007/s11214-020-00788-2] [Citation(s) in RCA: 6] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/20/2020] [Accepted: 12/26/2020] [Indexed: 05/27/2023]
Abstract
Nine simulations are used to predict the meteorology and aeolian activity of the Mars 2020 landing site region. Predicted seasonal variations of pressure and surface and atmospheric temperature generally agree. Minimum and maximum pressure is predicted at Ls ∼ 145 ∘ and 250 ∘ , respectively. Maximum and minimum surface and atmospheric temperature are predicted at Ls ∼ 180 ∘ and 270 ∘ , respectively; i.e., are warmest at northern fall equinox not summer solstice. Daily pressure cycles vary more between simulations, possibly due to differences in atmospheric dust distributions. Jezero crater sits inside and close to the NW rim of the huge Isidis basin, whose daytime upslope (∼east-southeasterly) and nighttime downslope (∼northwesterly) winds are predicted to dominate except around summer solstice, when the global circulation produces more southerly wind directions. Wind predictions vary hugely, with annual maximum speeds varying from 11 to 19 ms - 1 and daily mean wind speeds peaking in the first half of summer for most simulations but in the second half of the year for two. Most simulations predict net annual sand transport toward the WNW, which is generally consistent with aeolian observations, and peak sand fluxes in the first half of summer, with the weakest fluxes around winter solstice due to opposition between the global circulation and daytime upslope winds. However, one simulation predicts transport toward the NW, while another predicts fluxes peaking later and transport toward the WSW. Vortex activity is predicted to peak in summer and dip around winter solstice, and to be greater than at InSight and much greater than in Gale crater. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-020-00788-2.
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Affiliation(s)
| | - M. de la Torre Juárez
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91001 USA
| | - J. Pla-García
- Centro de Astrobiología (CSIC-INTA), 28850 Madrid, Spain
- Space Science Institute, Boulder, CO 80301 USA
| | | | | | - L. Neary
- Belgian Institute for Space Aeronomy, Brussels, Belgium
| | | | - F. Forget
- Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), 75005 Paris, France
| | - A. Spiga
- Laboratoire de Météorologie Dynamique/Institut Pierre Simon Laplace (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique (CNRS), École Polytechnique, École Normale Supérieure (ENS), 75005 Paris, France
- Institut Universitaire de France, 75005 Paris, France
| | | | - F. Daerden
- Belgian Institute for Space Aeronomy, Brussels, Belgium
| | - T. Bertrand
- Ames Research Center, Mountain View, CA USA
- LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 92195 Meudon, France
| | | | - R. Sullivan
- Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14853 USA
| | | | - B. Chide
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE), Toulouse, France
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3
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Threshold for sand mobility on Mars calibrated from seasonal variations of sand flux. Nat Commun 2014; 5:5096. [PMID: 25268931 DOI: 10.1038/ncomms6096] [Citation(s) in RCA: 82] [Impact Index Per Article: 8.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/29/2014] [Accepted: 08/28/2014] [Indexed: 11/08/2022] Open
Abstract
Coupling between surface winds and saltation is a fundamental factor governing geological activity and climate on Mars. Saltation of sand is crucial for both erosion of the surface and dust lifting into the atmosphere. Wind tunnel experiments along with measurements from surface meteorology stations and modelling of wind speeds suggest that winds should only rarely move sand on Mars. However, evidence for currently active dune migration has recently accumulated. Crucially, the frequency of sand-moving events and the implied threshold wind stresses for saltation have remained unknown. Here we present detailed measurements of Nili Patera dune field based on High Resolution Imaging Science Experiment images, demonstrating that sand motion occurs daily throughout much of the year and that the resulting sand flux is strongly seasonal. Analysis of the seasonal sand flux variation suggests an effective threshold for sand motion for application to large-scale model wind fields (1-100 km scale) of τ(s)=0.01±0.0015 N m(-2).
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Kok JF, Parteli EJR, Michaels TI, Karam DB. The physics of wind-blown sand and dust. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2012; 75:106901. [PMID: 22982806 DOI: 10.1088/0034-4885/75/10/106901] [Citation(s) in RCA: 160] [Impact Index Per Article: 13.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/12/2023]
Abstract
The transport of sand and dust by wind is a potent erosional force, creates sand dunes and ripples, and loads the atmosphere with suspended dust aerosols. This paper presents an extensive review of the physics of wind-blown sand and dust on Earth and Mars. Specifically, we review the physics of aeolian saltation, the formation and development of sand dunes and ripples, the physics of dust aerosol emission, the weather phenomena that trigger dust storms, and the lifting of dust by dust devils and other small-scale vortices. We also discuss the physics of wind-blown sand and dune formation on Venus and Titan.
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Affiliation(s)
- Jasper F Kok
- Department of Earth and Atmospheric Sciences, Cornell University, Ithaca, NY, USA.
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Arvidson RE, Ashley JW, Bell JF, Chojnacki M, Cohen J, Economou TE, Farrand WH, Fergason R, Fleischer I, Geissler P, Gellert R, Golombek MP, Grotzinger JP, Guinness EA, Haberle RM, Herkenhoff KE, Herman JA, Iagnemma KD, Jolliff BL, Johnson JR, Klingelhöfer G, Knoll AH, Knudson AT, Li R, McLennan SM, Mittlefehldt DW, Morris RV, Parker TJ, Rice MS, Schröder C, Soderblom LA, Squyres SW, Sullivan RJ, Wolff MJ. Opportunity Mars Rover mission: Overview and selected results from Purgatory ripple to traverses to Endeavour crater. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010je003746] [Citation(s) in RCA: 82] [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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Lichtenberg KA, Arvidson RE, Morris RV, Murchie SL, Bishop JL, Fernandez Remolar D, Glotch TD, Noe Dobrea E, Mustard JF, Andrews-Hanna J, Roach LH. Stratigraphy of hydrated sulfates in the sedimentary deposits of Aram Chaos, Mars. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003353] [Citation(s) in RCA: 63] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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7
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Edwards CS, Bandfield JL, Christensen PR, Fergason RL. Global distribution of bedrock exposures on Mars using THEMIS high-resolution thermal inertia. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003363] [Citation(s) in RCA: 65] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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8
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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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9
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Piqueux S, Christensen PR. North and south subice gas flow and venting of the seasonal caps of Mars: A major geomorphological agent. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003009] [Citation(s) in RCA: 53] [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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10
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Koeppen WC, Hamilton VE. Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002984] [Citation(s) in RCA: 169] [Impact Index Per Article: 10.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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11
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Hayward RK, Mullins KF, Fenton LK, Hare TM, Titus TN, Bourke MC, Colaprete A, Christensen PR. Mars Global Digital Dune Database and initial science results. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002943] [Citation(s) in RCA: 167] [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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12
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Kraal ER, Asphaug E, Moore JM, Lorenz RD. Quantitative geomorphic modeling of Martian bedrock shorelines. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002567] [Citation(s) in RCA: 21] [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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13
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Richardson MI, Mischna MA. Long-term evolution of transient liquid water on Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002367] [Citation(s) in RCA: 69] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Mark I. Richardson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - Michael A. Mischna
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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14
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Fenton LK. Aeolian processes in Proctor Crater on Mars: Mesoscale modeling of dune-forming winds. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002309] [Citation(s) in RCA: 62] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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15
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16
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Strausberg MJ. Observations of the initiation and evolution of the 2001 Mars global dust storm. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2004je002361] [Citation(s) in RCA: 93] [Impact Index Per Article: 4.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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17
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18
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Fenton LK, Bandfield JL, Ward AW. Aeolian processes in Proctor Crater on Mars: Sedimentary history as analyzed from multiple data sets. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je002015] [Citation(s) in RCA: 86] [Impact Index Per Article: 4.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Lori K. Fenton
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - Joshua L. Bandfield
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
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19
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Toigo AD, Richardson MI. Meteorology of proposed Mars Exploration Rover landing sites. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2003je002064] [Citation(s) in RCA: 37] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Anthony D. Toigo
- Center for Radiophysics and Space Research; Cornell University; Ithaca New York USA
| | - Mark I. Richardson
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
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20
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Treiman AH. Geologic settings of Martian gullies: Implications for their origins. ACTA ACUST UNITED AC 2003. [DOI: 10.1029/2002je001900] [Citation(s) in RCA: 164] [Impact Index Per Article: 7.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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21
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Richardson MI, Wilson RJ. A topographically forced asymmetry in the martian circulation and climate. Nature 2002; 416:298-301. [PMID: 11907570 DOI: 10.1038/416298a] [Citation(s) in RCA: 111] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
Abstract
Large seasonal and hemispheric asymmetries in the martian climate system are generally ascribed to variations in solar heating associated with orbital eccentricity. As the orbital elements slowly change (over a period of >104 years), characteristics of the climate such as dustiness and the vigour of atmospheric circulation are thought to vary, as should asymmetries in the climate (for example, the deposition of water ice at the northern versus the southern pole). Such orbitally driven climate change might be responsible for the observed layering in Mars' polar deposits by modulating deposition of dust and water ice. Most current theories assume that climate asymmetries completely reverse as the angular distance between equinox and perihelion changes by 180 degrees. Here we describe a major climate mechanism that will not precess in this way. We show that Mars' global north-south elevation difference forces a dominant southern summer Hadley circulation that is independent of perihelion timing. The Hadley circulation, a tropical overturning cell responsible for trade winds, largely controls interhemispheric transport of water and the bulk dustiness of the atmosphere. The topography therefore imprints a strong handedness on climate, with water ice and the active formation of polar layered deposits more likely in the north.
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Affiliation(s)
- Mark I Richardson
- Division of Geological and Planetary Sciences, California Institute of Technology, MC 150-21, Pasadena, California 91125, USA.
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22
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Richardson MI. Investigation of the nature and stability of the Martian seasonal water cycle with a general circulation model. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001536] [Citation(s) in RCA: 134] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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