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Wilson CF, Marcq E, Gillmann C, Widemann T, Korablev O, Mueller NT, Lefèvre M, Rimmer PB, Robert S, Zolotov MY. Possible Effects of Volcanic Eruptions on the Modern Atmosphere of Venus. SPACE SCIENCE REVIEWS 2024; 220:31. [PMID: 38585189 PMCID: PMC10997549 DOI: 10.1007/s11214-024-01054-5] [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: 04/26/2023] [Accepted: 02/01/2024] [Indexed: 04/09/2024]
Abstract
This work reviews possible signatures and potential detectability of present-day volcanically emitted material in the atmosphere of Venus. We first discuss the expected composition of volcanic gases at present time, addressing how this is related to mantle composition and atmospheric pressure. Sulfur dioxide, often used as a marker of volcanic activity in Earth's atmosphere, has been observed since late 1970s to exhibit variability at the Venus' cloud tops at time scales from hours to decades; however, this variability may be associated with solely atmospheric processes. Water vapor is identified as a particularly valuable tracer for volcanic plumes because it can be mapped from orbit at three different tropospheric altitude ranges, and because of its apparent low background variability. We note that volcanic gas plumes could be either enhanced or depleted in water vapor compared to the background atmosphere, depending on magmatic volatile composition. Non-gaseous components of volcanic plumes, such as ash grains and/or cloud aerosol particles, are another investigation target of orbital and in situ measurements. We discuss expectations of in situ and remote measurements of volcanic plumes in the atmosphere with particular focus on the upcoming DAVINCI, EnVision and VERITAS missions, as well as possible future missions.
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Affiliation(s)
- Colin F. Wilson
- European Space Agency, Keplerlaan 1, 2201, AZ Noordwijk, The Netherlands
- Physics Dept, Oxford University, Oxford, OX1 3PU UK
| | - Emmanuel Marcq
- LATMOS/IPSL, UVSQ Sorbonne Université Paris-Saclay, Sorbonne Université, CNRS, Guyancourt, France
| | - Cédric Gillmann
- Institut für Geophysik, Geophysical Fluid Dynamics, ETH Zurich, Sonneggstraße 5, 8092 Zürich, Switzerland
| | - Thomas Widemann
- LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
- Université Paris-Saclay, UVSQ, DYPAC, 78000 Versailles, France
| | - Oleg Korablev
- Space Research Institute (IKI), Russian Academy of Sciences, Moscow, 117997 Russia
| | - Nils T. Mueller
- Institute for Planetary Research, DLR, Rutherfordstraße 2, 12489 Berlin, Germany
- Institute of Geosciences, Freie Universität Berlin, Malteserstr. 74-100, 12249 Berlin, Germany
| | - Maxence Lefèvre
- LATMOS/IPSL, UVSQ Sorbonne Université Paris-Saclay, Sorbonne Université, CNRS, Guyancourt, France
| | - Paul B. Rimmer
- Cavendish Laboratory, University of Cambridge, JJ Thomson Avenue, Cambridge, CB3 0HE UK
| | - Séverine Robert
- Royal Belgian Institute for Space Aeronomy, Brussels, Belgium
| | - Mikhail Y. Zolotov
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404 USA
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Herrick RR, Hensley S. Surface changes observed on a Venusian volcano during the Magellan mission. Science 2023; 379:1205-1208. [PMID: 36921020 DOI: 10.1126/science.abm7735] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/17/2023]
Abstract
Venus has a geologically young surface, but it is unknown whether it has ongoing active volcanism. From 1990 to 1992, the Magellan spacecraft imaged the planet's surface, using synthetic aperture radar. We examined volcanic areas on Venus that were imaged two or three times by Magellan and identified an ~2.2-square-kilometer volcanic vent that changed shape in the 8-month interval between two radar images. Additional volcanic flows downhill from the vent are visible in the second-epoch images, although we cannot rule out that they were present but invisible in the first epoch because of differences in imaging geometry. We interpret these results as evidence of ongoing volcanic activity on Venus.
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Affiliation(s)
- Robert R Herrick
- Geophysical Institute, University of Alaska Fairbanks, Fairbanks, AK 99775, USA
| | - Scott Hensley
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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Brossier J, Gilmore MS, Toner K, Stein AJ. Distinct Mineralogy and Age of Individual Lava Flows in Atla Regio, Venus Derived From Magellan Radar Emissivity. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2021; 126:e2020JE006722. [PMID: 33959469 PMCID: PMC8098063 DOI: 10.1029/2020je006722] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/02/2020] [Accepted: 02/18/2021] [Indexed: 06/12/2023]
Abstract
NASA's Magellan mission revealed that many Venus highlands exhibit low radar emissivity values at higher altitudes. This phenomenon is ascribed to the presence of minerals having high dielectric constants, produced or stabilized by temperature-dependent chemical weathering between the rocks and the atmosphere. Some large volcanoes on Venus have multiple reductions of radar emissivity at varying altitudes. The authors present morphological maps of major lava flow units at Maat, Ozza, and Sapas montes and compare them to radar emissivity. Sapas has a single reduction in emissivity values at 6,054.6 km, while Maat and Ozza have several reductions at altitudes of 6,052.5-6,056.7 km. Emissivity values are highly spatially correlated to individual lava flows indicating that minerals in the rocks control the emissivity signature. The emissivity patterns at these volcanoes require at least four individual ferroelectric mineral compositions in the rocks that are highly conductive at Curie temperatures of 693-731 K. These temperatures are compatible with chlorapatite and some perovskite oxides. Modeling the minimum volumes of ferroelectrics (10-100s ppm) shows the volume and type of ferroelectric may vary over the lifetime of a single volcano. The modeled volumes of ferroelectrics in Ozza and Sapas are greater than in Maat, consistent with the production of ferroelectrics via weathering over a longer period of time, and supporting the idea that Maat has younger volcanic activity. The stratigraphic relationship of Maat's youngest flows with impact craters may indicate the timeframe of the production of specific ferroelectrics via chemical weathering is over 9-60 Ma.
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Affiliation(s)
- J. Brossier
- Department of Earth and Environmental Sciences, Planetary Sciences Group, Wesleyan University, Middletown, CT, USA
| | - M. S. Gilmore
- Department of Earth and Environmental Sciences, Planetary Sciences Group, Wesleyan University, Middletown, CT, USA
| | - K. Toner
- Department of Earth and Environmental Sciences, Planetary Sciences Group, Wesleyan University, Middletown, CT, USA
| | - A. J. Stein
- Department of Earth and Environmental Sciences, Planetary Sciences Group, Wesleyan University, Middletown, CT, USA
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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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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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Hansen VL, López I. Geologic Map of Aphrodite Map Area (AMA; I-2476), Venus. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2020; 7:e2019EA001066. [PMID: 33134435 PMCID: PMC7583386 DOI: 10.1029/2019ea001066] [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: 12/26/2019] [Revised: 06/08/2020] [Accepted: 06/13/2020] [Indexed: 06/11/2023]
Abstract
We present a 1:10-M-scale geologic map of the Aphrodite Map Area (AMA) of Venus (0°N-57°S/60-80°E). Geologic mapping employed NASA Magellan synthetic aperture radar and altimetry data. The AMA geologic map, with detailed structural elements and geologic units covering over one eighth of Venus' surface, affords an important and unique perspective to test models of global-scale geologic processes through time. Geologic relations record a history inconsistent with global catastrophic resurfacing. The AMA displays 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 ancient era and Artemis superstructure, with a footprint covering more than 25% of the surface, are recorded in the Niobe Map Area to the north. The latter two eras likely overlap in time. The fracture zone domain, part of a globally extensive province, marks the most spatially focused tectonomagmatic domain within the AMA. Impact craters are both cut by and overprint fracture zone structures. Twelve percent of AMA impact craters that occur within the fracture zone domain predate or formed during fracture zone development. This observation indicates the relative youth of the fracture zone era and is consistent with the possibility that this domain remains geologically active. The AMA records a rich geologic history of large tract of the surface of Venus and provides an important framework to formulate new working hypotheses of Venus evolution and contribute to planning future studies of the surface of planets.
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Affiliation(s)
- V. L. Hansen
- Department of Earth and Environmental SciencesUniversity of Minnesota, DuluthDuluthMNUSA
| | - I. López
- Department of Biology and Geology, Physics and Inorganic Chemistry, Área de GeologíaUniversidad Rey Juan CarlosMóstoles, MadridSpain
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Hansen VL. Global tectonic evolution of Venus, from exogenic to endogenic over time, and implications for early Earth processes. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2018; 376:rsta.2017.0412. [PMID: 30275161 DOI: 10.1098/rsta.2017.0412] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 07/04/2018] [Indexed: 06/08/2023]
Abstract
Venus provides a rich arena in which to stretch one's tectonic imagination with respect to non-plate tectonic processes of heat transfer on an Earth-like planet. Venus is similar to Earth in density, size, inferred composition and heat budget. However, Venus' lack of plate tectonics and terrestrial surficial processes results in the preservation of a unique surface geologic record of non-plate tectonomagmatic processes. In this paper, I explore three global tectonic domains that represent changes in global conditions and tectonic regimes through time, divided respectively into temporal eras. Impactors played a prominent role in the ancient era, characterized by thin global lithosphere. The Artemis superstructure era highlights sublithospheric flow processes related to a uniquely large super plume. The fracture zone complex era, marked by broad zones of tectonomagmatic activity, witnessed coupled spreading and underthrusting, since arrested. These three tectonic regimes provide possible analogue models for terrestrial Archaean craton formation, continent formation without plate tectonics, and mechanisms underlying the emergence of plate tectonics. A bolide impact model for craton formation addresses the apparent paradox of both undepleted mantle and growth of Archaean crust, and recycling of significant Archaean crust to the mantle.This article is part of a discussion meeting issue 'Earth dynamics and the development of plate tectonics'.
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Affiliation(s)
- Vicki L Hansen
- Department of Earth and Environmental Sciences, University of Minnesota Duluth, 1114 Kirby Drive, Duluth, MN 55812, USA
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Herrick RR, Stahlke DL, Sharpton VL. Fine-scale Venusian topography from Magellan stereo data. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2012eo120002] [Citation(s) in RCA: 22] [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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