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Khawja S, Ernst RE, Samson C, Byrne PK, Ghail RC, MacLellan LM. Tesserae on Venus may preserve evidence of fluvial erosion. Nat Commun 2020; 11:5789. [PMID: 33188168 PMCID: PMC7666114 DOI: 10.1038/s41467-020-19336-1] [Citation(s) in RCA: 12] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/04/2020] [Accepted: 10/06/2020] [Indexed: 11/30/2022] Open
Abstract
Fluvial erosion is usually assumed to be absent on Venus, precluded by a high surface temperature of ~450 °C and supported by extensive uneroded volcanic flows. However, recent global circulation models suggest the possibility of Earth-like climatic conditions on Venus for much of its earlier history, prior to catastrophic runaway greenhouse warming. We observe that the stratigraphically oldest, geologically most complex units, tesserae, exhibit valley patterns morphologically similar to the patterns resulting from fluvial erosion on Earth. Given poor topographic resolution, we use an indirect technique to recognize valleys, based on the pattern of lava flooding of tesserae margins by adjacent plains volcanism. These observed valley patterns are attributed to primary geology, tectonic deformation, followed by fluvial erosion (and lesser wind erosion). This proposed fluvial erosion in tesserae provides support for climate models for a cool, wet climate on early Venus and could be an attractive research theme for future Venus missions. The authors here use Magellan data to interpret geomorphological features on Venus and present a strong hypothesis for fluvial erosion.
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Affiliation(s)
- S Khawja
- Department of Earth Sciences, Carleton University, 1125 Colonel By Drive, Ottawa, Ontario, K1S 5B6, Canada
| | - R E Ernst
- Department of Earth Sciences, Carleton University, 1125 Colonel By Drive, Ottawa, Ontario, K1S 5B6, Canada. .,Faculty of Geology and Geography, Tomsk State University, 36 Lenin Avenue, Tomsk, 634050, Russia.
| | - C Samson
- Department of Earth Sciences, Carleton University, 1125 Colonel By Drive, Ottawa, Ontario, K1S 5B6, Canada
| | - P K Byrne
- Department of Marine, Earth, and Atmospheric Sciences, North Carolina State University, Raleigh, NC, 27695, USA
| | - R C Ghail
- Department of Earth Sciences, Royal Holloway, University of London, Egham, TW20 0EX, UK
| | - L M MacLellan
- Department of Earth Sciences, Carleton University, 1125 Colonel By Drive, Ottawa, Ontario, K1S 5B6, Canada
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Boutle IA, Joshi M, Lambert FH, Mayne NJ, Lyster D, Manners J, Ridgway R, Kohary K. Mineral dust increases the habitability of terrestrial planets but confounds biomarker detection. Nat Commun 2020; 11:2731. [PMID: 32518292 PMCID: PMC7283277 DOI: 10.1038/s41467-020-16543-8] [Citation(s) in RCA: 12] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/09/2019] [Accepted: 05/05/2020] [Indexed: 11/09/2022] Open
Abstract
Identification of habitable planets beyond our solar system is a key goal of current and future space missions. Yet habitability depends not only on the stellar irradiance, but equally on constituent parts of the planetary atmosphere. Here we show, for the first time, that radiatively active mineral dust will have a significant impact on the habitability of Earth-like exoplanets. On tidally-locked planets, dust cools the day-side and warms the night-side, significantly widening the habitable zone. Independent of orbital configuration, we suggest that airborne dust can postpone planetary water loss at the inner edge of the habitable zone, through a feedback involving decreasing ocean coverage and increased dust loading. The inclusion of dust significantly obscures key biomarker gases (e.g. ozone, methane) in simulated transmission spectra, implying an important influence on the interpretation of observations. We demonstrate that future observational and theoretical studies of terrestrial exoplanets must consider the effect of dust. In this study, the authors investigate in the influence of atmospheric dust on the habitability of exoplanets. They find that atmospheric dust may postpone planetary water loss; for tidally locked planets in particular, dust can significantly widen the habitable zone by cooling the day side and warming the night side.
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Affiliation(s)
- Ian A Boutle
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK. .,Met Office, FitzRoy Road, Exeter, EX1 3PB, UK.
| | - Manoj Joshi
- School of Environmental Sciences, University of East Anglia, Norwich, NR4 7TJ, UK
| | - F Hugo Lambert
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK
| | - Nathan J Mayne
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK
| | - Duncan Lyster
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK
| | - James Manners
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK.,Met Office, FitzRoy Road, Exeter, EX1 3PB, UK
| | - Robert Ridgway
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK
| | - Krisztian Kohary
- College of Engineering, Mathematics and Physical Sciences, University of Exeter, Exeter, EX4 4QL, UK
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Abstract
Despite a very thin atmosphere, dunes may form on Pluto
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Affiliation(s)
- Alexander G Hayes
- Spacecraft Planetary Imaging Facility, Cornell University, 412 Space Science Building, Ithaca, NY 14853-6801, USA.
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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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Campbell BA, Morgan GA, Whitten JL, Carter LM, Glaze LS, Campbell DB. Pyroclastic Flow Deposits on Venus as Indicators of Renewed Magmatic Activity. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2017; Volume 122:1580-1596. [PMID: 31709132 PMCID: PMC6839737 DOI: 10.1002/2017je005299] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Radar-bright deposits on Venus that have diffuse margins suggest eruptions that distribute debris over large areas due to ground-hugging flows from plume collapse. We examine deposits in Eastern Eistla, Western Eistla, Phoebe, and Dione Regiones using Magellan data and Earth-based radar maps. The radar-bright units have no marginal lobes or other features consistent with viscous flow. Their morphology, radar echo strength, polarization properties, and microwave emissivity are consistent with mantling deposits comprised of few-cm or larger clasts. This debris traveled downhill up to ~100 km on modest slopes, and blanketed lava flows and tectonic features to depths of tens of cm to a few meters over areas up to 40×103 km2. There is evidence for ongoing removal and exhumation of previously buried terrain. A newly identified occurrence is associated with a ridge belt south of Ushas Mons. We also note radar-bright streaks of coarse material west of Rona Chasma that reflect the last traces of a deposit mobilized by winds from the formation of Mirabeau crater. If the radar-bright units originate by collapse of eruption columns, with coarse fragmental material entrained and fluidized by hot gases, then their extent suggests large erupted volatile (CO2 or H2O) amounts. We propose that these deposits reflect the early stage of renewed magmatic activity, with volatile-rich, disrupted magma escaping through vents in fractured regions of the upper crust. Rapidly eroding under Venus surface conditions, or buried by subsequent eruptions, these markers of recently renewed activity have disappeared from older regions.
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Affiliation(s)
- Bruce A. Campbell
- Center for Earth and Planetary Studies, Smithsonian Institution, MRC 315, PO Box 37012, Washington, DC 20013-7012, Phone: (202) 633-2472
| | - Gareth A. Morgan
- Center for Earth and Planetary Studies, Smithsonian Institution, MRC 315, PO Box 37012, Washington, DC 20013-7012, Phone: (202) 633-2472
| | - Jennifer L. Whitten
- Center for Earth and Planetary Studies, Smithsonian Institution, MRC 315, PO Box 37012, Washington, DC 20013-7012, Phone: (202) 633-2472
| | - Lynn M. Carter
- Lunar and Planetary Laboratory, 1629 E University Blvd., University of Arizona, Tucson, AZ 85721-0092
| | - Lori S. Glaze
- NASA Goddard Space Flight Center, Code 690, Greenbelt, MD 20771
| | - Donald B. Campbell
- Cornell University, Dept. of Astronomy, 502 Space Sciences Bldng., Ithaca, NY 14853
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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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Basilevsky AT. Impact crater air fall deposits on the surface of Venus: Areal distribution, estimated thickness, recognition in surface panoramas, and implications for provenance of sampled surface materials. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002307] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Bondarenko NV. Radar-dark impact crater–related parabolas on Venus: Characterization of deposits with Magellan emissivity data. ACTA ACUST UNITED AC 2004. [DOI: 10.1029/2004je002256] [Citation(s) in RCA: 22] [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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Snyder D. Cooling of lava flows on Venus: The coupling of radiative and convective heat transfer. ACTA ACUST UNITED AC 2002. [DOI: 10.1029/2001je001501] [Citation(s) in RCA: 20] [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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Collins GC, Head JW, Basilevsky AT, Ivanov MA. Evidence for rapid regional plains emplacement on Venus from the population of volcanically embayed impact craters. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1999je001041] [Citation(s) in RCA: 29] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Wichman RW. Internal crater modification on Venus: Recognizing crater-centered volcanism by changes in floor morphometry and floor brightness. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/1997je000428] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Bridges NT, Greeley R, Haldemann AFC, Herkenhoff KE, Kraft M, Parker TJ, Ward AW. Ventifacts at the Pathfinder landing site. ACTA ACUST UNITED AC 1999. [DOI: 10.1029/98je02550] [Citation(s) in RCA: 84] [Impact Index Per Article: 3.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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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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Greeley R, Schubert G, Limonadi D, Bender KC, Newman WI, Thomas PE, Weitz CM, Wall SD. Wind streaks on venus: clues to atmospheric circulation. Science 1994; 263:358-61. [PMID: 17769799 DOI: 10.1126/science.263.5145.358] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Magellan images reveal surface features on Venus attributed to wind processes. Sand dunes, wind-sculpted hills, and more than 5830 wind streaks have been identified. The streaks serve as local "wind vanes," representing wind direction at the time of streak formation and allowing the first global mapping of near-surface wind patterns on Venus. Wind streaks are oriented both toward the equator and toward the west. When streaks associated with local transient events, such as impact cratering, are deleted, the westward component is mostly lost but the equatorward component remains. This pattern is consistent with a Hadley circulation of the lower atmosphere.
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Campbell BA, Rogers PG. Bell Regio, Venus: Integration of remote sensing data and terrestrial analogs for geologic analysis. ACTA ACUST UNITED AC 1994. [DOI: 10.1029/94je01862] [Citation(s) in RCA: 27] [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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Saunders RS, Spear AJ, Allin PC, Austin RS, Berman AL, Chandlee RC, Clark J, Decharon AV, De Jong EM, Griffith DG, Gunn JM, Hensley S, Johnson WTK, Kirby CE, Leung KS, Lyons DT, Michaels GA, Miller J, Morris RB, Morrison AD, Piereson RG, Scott JF, Shaffer SJ, Slonski JP, Stofan ER, Thompson TW, Wall SD. Magellan mission summary. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je01397] [Citation(s) in RCA: 128] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Arvidson RE, Greeley R, Malin MC, Saunders RS, Izenberg N, Plaut JJ, Stofan ER, Shepard MK. Surface modification of Venus as inferred from Magellan observations of plains. ACTA ACUST UNITED AC 1992. [DOI: 10.1029/92je01384] [Citation(s) in RCA: 92] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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