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Love R, Jackson DWT, Michaels T, Smyth TAG, Avouac JP, Cooper A. From Macro- to Microscale: A combined modelling approach for near-surface wind flow on Mars at sub-dune length-scales. PLoS One 2022; 17:e0276547. [PMCID: PMC9635718 DOI: 10.1371/journal.pone.0276547] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/15/2022] [Accepted: 10/07/2022] [Indexed: 11/06/2022] Open
Abstract
The processes that initiate and sustain sediment transport which contribute to the modification of aeolian deposits in Mars’ low-density atmosphere are still not fully understood despite recent atmospheric modelling. However, detailed microscale wind flow modelling, using Computational Fluid Dynamics at a resolution of <2 m, provides insights into the near-surface processes that cannot be modeled using larger-scale atmospheric modeling. Such Computational Fluid Dynamics simulations cannot by themselves account for regional-scale atmospheric circulations or flow modifications induced by regional km-scale topography, although realistic fine-scale mesoscale atmospheric modeling can. Using the output parameters from mesoscale simulations to inform the input conditions for the Computational Fluid Dynamics microscale simulations provides a practical approach to simulate near-surface wind flow and its relationship to very small-scale topographic features on Mars, particularly in areas which lack in situ rover data. This paper sets out a series of integrated techniques to enable a multi-scale modelling approach for surface airflow to derive surface airflow dynamics at a (dune) landform scale using High Resolution Imaging Science Experiment derived topographic data. The work therefore provides a more informed and realistic Computational Fluid Dynamics microscale modelling method, which will provide more detailed insight into the surface wind forcing of aeolian transport patterns on martian surfaces such as dunes.
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Affiliation(s)
- Richard Love
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- * E-mail:
| | - Derek W. T. Jackson
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- Geological Sciences, University of KwaZulu-Natal, Durban, South Africa
| | - Timothy Michaels
- Carl Sagan Center (at the SETI Institute), Mountain View, California, United States of America
| | - Thomas A. G. Smyth
- Department of Biological and Geographical Sciences, School of Applied Sciences, University of Huddersfield, England, United Kingdom
| | - Jean-Philippe Avouac
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- Division of Geological and Planetary Sciences, CalTech, Pasadena, California, United States of America
| | - Andrew Cooper
- School of Geography & Environmental Sciences, Ulster University, Northern Ireland, United Kingdom
- Geological Sciences, University of KwaZulu-Natal, Durban, South Africa
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McKeeby BE, Ramsey MS, Tai Udovicic CJ, Haberle C, Edwards CS. Quantifying Sub-Meter Surface Heterogeneity on Mars Using Off-Axis Thermal Emission Imaging System (THEMIS) Data. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2022; 9:e2022EA002430. [PMID: 36588669 PMCID: PMC9788145 DOI: 10.1029/2022ea002430] [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: 05/16/2022] [Revised: 07/26/2022] [Accepted: 08/03/2022] [Indexed: 06/17/2023]
Abstract
Surface heterogeneities below the spatial resolution of thermal infrared (TIR) instruments result in anisothermality and can produce emissivity spectra with negative slopes toward longer wavelengths. Sloped spectra arise from an incorrect assumption of either a uniform surface temperature or a maximum emissivity during the temperature-emissivity separation of radiance data. Surface roughness and lateral mixing of different sub-pixel surface units result in distinct spectral slopes with magnitudes proportional to the degree of temperature mixing. Routine Off-nadir Targeted Observations (ROTO) of the Thermal Emission Imaging Spectrometer (THEMIS) are used here for the first time to investigate anisothermality below the spatial resolution of THEMIS. The southern flank of Apollinaris Mons and regions within the Medusae Fossae Formation are studied using THEMIS ROTO data acquired just after local sunset. We observe a range of sloped TIR emission spectra dependent on the magnitude of temperature differences within a THEMIS pixel. Spectral slopes and wavelength-dependent brightness temperature differences are forward-modeled for a series of two-component surfaces of varying thermal inertia values. Our results imply that differing relative proportions of rocky and unconsolidated surface units are observed at each ROTO viewing geometry and suggest a local rock abundance six times greater than published results that rely on nadir data. High-resolution visible images of these regions indicate a mixture of surface units from boulders to dunes, providing credence to the model.
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Affiliation(s)
- B. E. McKeeby
- Department of Geology and Environmental ScienceUniversity of PittsburghPittsburghPAUSA
| | - M. S. Ramsey
- Department of Geology and Environmental ScienceUniversity of PittsburghPittsburghPAUSA
| | - C. J. Tai Udovicic
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - C. Haberle
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - C. S. Edwards
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
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Abstract
Transverse aeolian ridges (TARs) are poorly understood relict aeolian Martian surface features. Processes that create TARs are not well-constrained, and understanding their formation is complicated since they appear to share some features of ripples, megaripples, and dunes. While some evidence of multi-stage TAR formation has been documented in Nirgal Vallis, here we present additional evidence for this process at nine locations on Mars using cratering superposition between different ridge morphologies. Most occurrences of multistage evolution will not preserve the precise series of cratering and formation events documented here, which potentially means that this formative process may have been more common than even these new widespread observations suggest. This formative process can help determine the relative similarity of TARs to ripples, megaripples and dunes. Based on our observations, we conclude that primary TAR forms are most like megaripples, and that subsequent ridges formed like aqueous ripple spurs.
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Silvestro S, Chojnacki M, Vaz DA, Cardinale M, Yizhaq H, Esposito F. Megaripple Migration on Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2020; 125:e2020JE006446. [PMID: 33133993 PMCID: PMC7583471 DOI: 10.1029/2020je006446] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/10/2020] [Revised: 06/09/2020] [Accepted: 06/12/2020] [Indexed: 06/11/2023]
Abstract
Aeolian megaripples, with 5- to 50-m spacing, are abundant on the surface of Mars. These features were repeatedly targeted by high-resolution orbital images, but they have never been observed to move. Thus, aeolian megaripples (especially the bright-toned ones often referred as Transverse Aeolian Ridges-TARs) have been interpreted as relict features of a past climate. In this report, we show evidence for the migration of bright-toned megaripples spaced 1 to 35 m (5 m on average) in two equatorial areas on Mars indicating that megaripples and small TARs can be active today. The moving megaripples display sand fluxes that are 2 orders of magnitudes lower than the surrounding dunes on average and, unlike similar bedforms on Earth, can migrate obliquely and longitudinally. In addition, the active megaripples in the two study areas of Syrtis Major and Mawrth Vallis show very similar flux distributions, echoing the similarities between dune crest fluxes in the two study areas and suggesting the existence of a relationship between dune and megaripple fluxes that can be explored elsewhere. Active megaripples, together with high-sand flux dunes, represent a key indicator of strong winds at the surface of Mars. A past climate with a denser atmosphere is not necessary to explain their accumulation and migration.
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Affiliation(s)
- S. Silvestro
- INAF Osservatorio Astronomico di CapodimonteNapoliItaly
- SETI InstituteMountain ViewCAUSA
| | - M. Chojnacki
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
- Planetary Science InstituteTucsonAZUSA
| | - D. A. Vaz
- Centre for Earth and Space Research of the University of CoimbraObservatório Geofísico e Astronómico da Universidade de CoimbraCoimbraPortugal
| | | | - H. Yizhaq
- Department of Solar Energy and Environmental Physics, BIDRBen‐Gurion University of the NegevBeershebaIsrael
| | - F. Esposito
- INAF Osservatorio Astronomico di CapodimonteNapoliItaly
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Ewing RC, Lapotre MGA, Lewis KW, Day M, Stein N, Rubin DM, Sullivan R, Banham S, Lamb MP, Bridges NT, Gupta S, Fischer WW. Sedimentary processes of the Bagnold Dunes: Implications for the eolian rock record of Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2017; 122:2544-2573. [PMID: 29497590 PMCID: PMC5815379 DOI: 10.1002/2017je005324] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/10/2017] [Revised: 06/19/2017] [Accepted: 06/26/2017] [Indexed: 05/31/2023]
Abstract
The Mars Science Laboratory rover Curiosity visited two active wind-blown sand dunes within Gale crater, Mars, which provided the first ground-based opportunity to compare Martian and terrestrial eolian dune sedimentary processes and study a modern analog for the Martian eolian rock record. Orbital and rover images of these dunes reveal terrestrial-like and uniquely Martian processes. The presence of grainfall, grainflow, and impact ripples resembled terrestrial dunes. Impact ripples were present on all dune slopes and had a size and shape similar to their terrestrial counterpart. Grainfall and grainflow occurred on dune and large-ripple lee slopes. Lee slopes were ~29° where grainflows were present and ~33° where grainfall was present. These slopes are interpreted as the dynamic and static angles of repose, respectively. Grain size measured on an undisturbed impact ripple ranges between 50 μm and 350 μm with an intermediate axis mean size of 113 μm (median: 103 μm). Dissimilar to dune eolian processes on Earth, large, meter-scale ripples were present on all dune slopes. Large ripples had nearly symmetric to strongly asymmetric topographic profiles and heights ranging between 12 cm and 28 cm. The composite observations of the modern sedimentary processes highlight that the Martian eolian rock record is likely different from its terrestrial counterpart because of the large ripples, which are expected to engender a unique scale of cross stratification. More broadly, however, in the Bagnold Dune Field as on Earth, dune-field pattern dynamics and basin-scale boundary conditions will dictate the style and distribution of sedimentary processes.
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Affiliation(s)
- R. C. Ewing
- Department of Geology and GeophysicsTexas A&M UniversityCollege StationTexasUSA
| | - M. G. A. Lapotre
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCaliforniaUSA
| | - K. W. Lewis
- Department of Earth and Planetary SciencesJohns Hopkins UniversityBaltimoreMarylandUSA
| | - M. Day
- Jackson School of Geosciences, Department of Geological SciencesUniversity of Texas at AustinAustinTexasUSA
| | - N. Stein
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCaliforniaUSA
| | - D. M. Rubin
- Department of Earth and Planetary SciencesUniversity of CaliforniaSanta CruzCaliforniaUSA
| | - R. Sullivan
- Department of AstronomyCornell UniversityIthacaNew YorkUSA
| | - S. Banham
- Department of Earth Science and EngineeringImperial College LondonLondonUK
| | - M. P. Lamb
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCaliforniaUSA
| | - N. T. Bridges
- The Johns Hopkins University Applied Physics LaboratoryLaurelMarylandUSA
| | - S. Gupta
- Department of Earth Science and EngineeringImperial College LondonLondonUK
| | - W. W. Fischer
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCaliforniaUSA
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Raack J, Conway SJ, Herny C, Balme MR, Carpy S, Patel MR. Water induced sediment levitation enhances downslope transport on Mars. Nat Commun 2017; 8:1151. [PMID: 29075001 PMCID: PMC5658360 DOI: 10.1038/s41467-017-01213-z] [Citation(s) in RCA: 28] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/22/2017] [Accepted: 08/30/2017] [Indexed: 11/12/2022] Open
Abstract
On Mars, locally warm surface temperatures (~293 K) occur, leading to the possibility of (transient) liquid water on the surface. However, water exposed to the martian atmosphere will boil, and the sediment transport capacity of such unstable water is not well understood. Here, we present laboratory studies of a newly recognized transport mechanism: “levitation” of saturated sediment bodies on a cushion of vapor released by boiling. Sediment transport where this mechanism is active is about nine times greater than without this effect, reducing the amount of water required to transport comparable sediment volumes by nearly an order of magnitude. Our calculations show that the effect of levitation could persist up to ~48 times longer under reduced martian gravity. Sediment levitation must therefore be considered when evaluating the formation of recent and present-day martian mass wasting features, as much less water may be required to form such features than previously thought. Downslope sediment transport on Mars is reported, but the transport capacity of unstable water under low pressures is not well understood. Here, the authors present a newly discovered, highly reactive transportation mechanism that is only possible under low pressure environments.
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Affiliation(s)
- Jan Raack
- School of Physical Sciences, Faculty of Science, Technology, Engineering & Mathematics, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK.
| | - Susan J Conway
- Laboratoire de Planétologie et Géodynamique-UMR CNRS 6112, Université de Nantes, 2 rue de la Houssinière-BP 92208, 44322, Nantes Cedex 3, France
| | - Clémence Herny
- Physikalisches Institut, Universität Bern, Sidlerstrasse 5, 3012, Bern, Switzerland
| | - Matthew R Balme
- School of Physical Sciences, Faculty of Science, Technology, Engineering & Mathematics, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
| | - Sabrina Carpy
- Laboratoire de Planétologie et Géodynamique-UMR CNRS 6112, Université de Nantes, 2 rue de la Houssinière-BP 92208, 44322, Nantes Cedex 3, France
| | - Manish R Patel
- School of Physical Sciences, Faculty of Science, Technology, Engineering & Mathematics, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK.,Space Science and Technology Department, STFC Rutherford Appleton Laboratory, Harwell Campus, Didcot, OX11 0QX, UK
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7
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Anderson W, Day M. Turbulent flow over craters on Mars: Vorticity dynamics reveal aeolian excavation mechanism. Phys Rev E 2017; 96:043110. [PMID: 29347578 DOI: 10.1103/physreve.96.043110] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/03/2017] [Indexed: 06/07/2023]
Abstract
Impact craters are scattered across Mars. These craters exhibit geometric self-similarity over a spectrum of diameters, ranging from tens to thousands of kilometers. The late Noachian-early Hesperian boundary marks a dramatic shift in the role of mid-latitude craters, from depocenter sedimentary basins to aeolian source areas. At present day, many craters contain prominent layered sedimentary mounds with maximum elevations comparable to the rim height. The mounds are remnants of Noachian deposition and are surrounded by a radial moat. Large-eddy simulation has been used to model turbulent flows over synthetic craterlike geometries. Geometric attributes of the craters and the aloft flow have been carefully matched to resemble ambient conditions in the atmospheric boundary layer of Mars. Vorticity dynamics analysis within the crater basin reveals the presence of counterrotating helical vortices, verifying the efficacy of deflationary models put forth recently by Bennett and Bell [K. Bennett and J. Bell, Icarus 264, 331 (2016)]ICRSA50019-103510.1016/j.icarus.2015.09.041 and Day et al. [M. Day et al., Geophys. Res. Lett. 43, 2473 (2016)]GPRLAJ0094-827610.1002/2016GL068011. We show how these helical counterrotating vortices spiral around the outer rim, gradually deflating the moat and carving the mound; excavation occurs faster on the upwind side, explaining the radial eccentricity of the mounds relative to the surrounding crater basin.
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Affiliation(s)
- William Anderson
- Department of Mechanical Engineering, University of Texas at Dallas, Richardson, Texas 75080, USA
| | - Mackenzie Day
- Department of Earth and Space Sciences, University of Washington, 4000 15th Ave NE, Seattle, Washington 98195, USA
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8
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Hanna RD, Hamilton VE, Putzig NE. The complex relationship between olivine abundance and thermal inertia on Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2016; 121:1293-1320. [PMID: 31007993 PMCID: PMC6469700 DOI: 10.1002/2015je004924] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We examine four olivine-bearing regions at a variety of spatial scales with thermal infrared, visible to near-infrared, and visible imagery data to investigate the hypothesis that the relationship between olivine abundance and thermal inertia (i.e., effective particle size) can be used to infer the occurrence of olivine chemical alteration during sediment production on Mars. As in previous work, Nili Fossae and Isidis Planitia show a positive correlation between thermal inertia and olivine abundance in Thermal Emission Spectrometer (TES) and Thermal Emission Imaging System (THEMIS) data, which could be interpreted as indicating olivine chemical weathering. However, geomorphological analysis reveals that relatively olivine-poor sediments are not derived from adjacent olivine-rich materials, and therefore, chemical weathering cannot be inferred based on the olivine-thermal inertia relationship alone. We identify two areas (Terra Cimmeria and Argyre Planitia) with significant olivine abundance and thermal inertias consistent with sand, but no adjacent rocky (parent) units having even greater olivine abundances. More broadly, global analysis with TES reveals that the most typical olivine abundance on Mars is ~5-7% and that olivine-bearing (5-25%) materials have a wide range of thermal inertias, commonly 25-600 J m-2 K-1 s-1/2. TES also indicates that the majority of olivine-rich (>25%) materials have apparent thermal inertias less than 400 J m-2 K-1 s-1/2. In summary, we find that the relationship between thermal inertia and olivine abundance alone cannot be used in infer olivine weathering in the examined areas, that olivine-bearing materials have a large range of thermal intertias, and therefore that a complex relationship between olivine abundance and thermal inertia exists on Mars.
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Affiliation(s)
- Romy D Hanna
- Jackson School of Geological Sciences, University of Texas at Austin, Austin, Texas, USA
| | - Victoria E Hamilton
- Department of Space Studies, Southwest Research Institute, Boulder, Colorado, USA
| | - Nathaniel E Putzig
- Department of Space Studies, Southwest Research Institute, Boulder, Colorado, USA
- Now at the Planetary Science Institute, Lakewood, Colorado, USA
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9
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Satellite-Based Thermophysical Analysis of Volcaniclastic Deposits: A Terrestrial Analog for Mantled Lava Flows on Mars. REMOTE SENSING 2016. [DOI: 10.3390/rs8020152] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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10
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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: 158] [Impact Index Per Article: 13.2] [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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12
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Tirsch D, Jaumann R, Pacifici A, Poulet F. Dark aeolian sediments in Martian craters: Composition and sources. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2009je003562] [Citation(s) in RCA: 62] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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13
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Hayward RK, Titus TN, Michaels TI, Fenton LK, Colaprete A, Christensen PR. Aeolian dunes as ground truth for atmospheric modeling on Mars. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003428] [Citation(s) in RCA: 41] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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14
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Thomson BJ, Bridges NT, Greeley R. Rock abrasion features in the Columbia Hills, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003018] [Citation(s) in RCA: 25] [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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15
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Sullivan R, Arvidson R, Bell JF, Gellert R, Golombek M, Greeley R, Herkenhoff K, Johnson J, Thompson S, Whelley P, Wray J. Wind-driven particle mobility on Mars: Insights from Mars Exploration Rover observations at “El Dorado” and surroundings at Gusev Crater. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003101] [Citation(s) in RCA: 220] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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16
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McDowell ML, Hamilton VE. Geologic characteristics of relatively high thermal inertia intracrater deposits in southwestern Margaritifer Terra, Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2007je002925] [Citation(s) in RCA: 15] [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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17
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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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18
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Parteli EJR, Herrmann HJ. Dune formation on the present Mars. PHYSICAL REVIEW. E, STATISTICAL, NONLINEAR, AND SOFT MATTER PHYSICS 2007; 76:041307. [PMID: 17994981 DOI: 10.1103/physreve.76.041307] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/01/2007] [Revised: 08/09/2007] [Indexed: 05/25/2023]
Abstract
We apply a model for sand dunes to calculate formation of dunes on Mars under the present Martian atmospheric conditions. We find that different dune shapes as those imaged by Mars Global Surveyor could have been formed by the action of sand-moving winds occurring on today's Mars. Our calculations show, however, that Martian dunes could be only formed due to the higher efficiency of Martian winds in carrying grains into saltation. The model equations are solved to study saltation transport under different atmospheric conditions valid for Mars. We obtain an estimate for the wind speed and migration velocity of barchan dunes at different places on Mars. From comparison with the shape of bimodal sand dunes, we find an estimate for the time scale of the changes in Martian wind regimes.
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Affiliation(s)
- Eric J R Parteli
- Institut für Computerphysik, ICP, Universität Stuttgart, Pfaffenwaldring 27, 70569 Stuttgart, Germany
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19
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Rogers AD, Bandfield JL, Christensen PR. Global spectral classification of Martian low-albedo regions with Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) data. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002726] [Citation(s) in RCA: 56] [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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20
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Fergason RL, Christensen PR, Bell JF, Golombek MP, Herkenhoff KE, Kieffer HH. Physical properties of the Mars Exploration Rover landing sites as inferred from Mini-TES-derived thermal inertia. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002583] [Citation(s) in RCA: 114] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Robin L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - James F. Bell
- Department of Astronomy, Space Science Building; Cornell University; Ithaca New York USA
| | - Matthew P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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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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22
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Kleinhans MG. Flow discharge and sediment transport models for estimating a minimum timescale of hydrological activity and channel and delta formation on Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002521] [Citation(s) in RCA: 126] [Impact Index Per Article: 6.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Bourke MC. Aeolian sediment transport pathways and aerodynamics at troughs on Mars. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2003je002155] [Citation(s) in RCA: 50] [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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25
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Wilson SA. Latitude-dependent nature and physical characteristics of transverse aeolian ridges on Mars. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002247] [Citation(s) in RCA: 80] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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