Solid Planet–Atmosphere Interactions

Zolotov, M. Yu.

doi:10.1016/b978-044452748-6.00181-4

Cited by 6 publications

(6 citation statements)

References 126 publications

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“…We also exposed basaltic and andesitic glasses, common in terrestrial basalts. Whether or not they exist on Venus' surface has yet to be determined, but amorphous geologic materials have previously been suggested to be highly reactive on Venus' surface (e.g., Zolotov, 2007) and shown to form a variety of complex secondary minerals when exposed to sulfur‐bearing gases in previous work (Ayris et al., 2013; Berger et al., 2019; Burnett et al., 1997; Henley et al., 2015; Johnson & Burnett, 1993; Palm et al., 2018; Renggli & King, 2018; Treiman & Allen, 1994). Exposed glasses in our experiments included BHVO‐2G (USGS microanalysis standard basaltic glass), Halema'uma'u Spatter glass, AGV‐2G (USGS microanalysis standard andesitic glass), and synthetic glass with Venera 13 lander oxide abundances manufactured specifically for this study to represent Venus surface simulant.…”

Section: Methodsmentioning

confidence: 99%

Experiments on the reactivity of basaltic minerals and glasses in Venus surface conditions using the Glenn Extreme Environment Rig

Radoman-Shaw

Harvey

Costa

et al. 2022

Meteorit & Planetary Scien

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Climate models for Venus rely heavily on theoretical modeling and laboratory experimentation due to the extreme surface conditions of the planet and limited in situ surface data. To better explore the relative importance of reactions between the surface and the atmosphere on Venus, we exposed representative volcanic glasses and basaltic minerals to a large‐scale simulation of Venus surface conditions with a realistic atmospheric composition. This study consistend of two experiments of 42 and 80 days that replicated both physical conditions and atmosphere composition derived from available in situ near‐surface data using the Glenn Extreme Environment Rig (GEER) at the NASA Glenn Research Center. These experiments revealed significant reactivity of common Ca‐bearing pyroxenes (diopside and augite) to form anhydrite. Olivine and labradorite showed minimal reactivity. Volcanic glasses, including both natural and synthetic samples, were exceptionally reactive, rapidly forming both anhydrite and thénardite (Na2SO4), as well as transition metal sulfates (i.e., Cu, Cr), halite (NaCl), and sylvite (KCl). Our results document chemical and textural alteration of sample surfaces and provide sufficient evidence for an active sulfur sink on multiple samples, with sulfates as the dominant secondary mineralogy. These experiments suggest likely surface mineralogies and solid phases present on Venus' surface with significant implications for upcoming missions and provide new data for comparison to high‐temperature mineral–gas reactions prevalent on Venus, Earth, and Io.

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Section: Methodsmentioning

confidence: 99%

Experiments on the reactivity of basaltic minerals and glasses in Venus surface conditions using the Glenn Extreme Environment Rig

Radoman-Shaw

Harvey

Costa

et al. 2022

Meteorit & Planetary Scien

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“…Magnetite is unstable on the surface—oxidizing to hematite via the reduction of carbon dioxide to carbon monoxide—except possibly at low elevations (Fegley et al, ; Zolotov, ). Weathering that occurs after a putative dynamo dies tends to remove extant TRM (i.e., by acquiring chemical remanent magnetization in zero field).…”

Section: Possible Magnetic Signals From the Surfacementioning

confidence: 99%

Detectability of Remanent Magnetism in the Crust of Venus

O’Rourke

Buz

et al. 2019

Geophysical Research Letters

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Observations of planetary magnetic fields provide fundamental insights into the origin and evolution of terrestrial planets. However, whether Venus ever hosted a dynamo is unknown. Here we show that crustal remanent magnetism is a potentially observable consequence of an ancient Venusian dynamo, in contrast to previous studies that dismissed this possibility. Past spacecraft measurements only exclude crustal magnetization near the Venera 4 landing site and northward of 50° South latitude for >150‐km coherence scales and strong magnetization intensities. Magnetite grains with sizes commonly observed in volcanic rocks can retain thermoremanent magnetism at Venusian conditions for >1 billion years. Depths to the Curie temperature of magnetite are ~5–40 km and typically less than predicted crustal thicknesses at our analyzed localities. Aerial platforms could detect expected magnetizations at horizontal scales similar to the ~50‐km operating altitude. Any detection would validate models of planetary accretion, geologic processes, and climate history.

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“…However, hydration reactions may also produce H 2 gas as a by-product which can potentially escape and allow progressive oxidation of the planet. Additional weathering reactions involve trace gases such as SO 2 , HCl, and HF, which can produce sulfates as well as chloride and fluoride salts, and are important on both Mars and Venus, but these are expected to have less of a role on climate, so we refer the reader to the review by Zolotov (2007) for further details.…”

Section: Surface Weathering Reactionsmentioning

confidence: 99%

“…At present, the carbonate-silicate cycle does not operate on Venus due to the high surface temperature and low water abundance. Rather, Venus may at present have a high enough surface temperature for mineral reactions to buffer the abundances of some atmospheric gases, although this model has been disputed in recent years (see reviews in Gilmore et al, 2017, Zolotov, 2007 and there is at present no evidence for major gas sinks in Venus' lower atmosphere. However, the past history of surface-atmosphere interactions on Venus is not well studied, in the wet early Venus scenario.…”

Section: Surface Weathering Reactionsmentioning

confidence: 99%

“…Venus' surface is sufficiently young that massive carbonates are not expected to have survived resurfacing, although they could potentially be preserved in the tessera terrain if it is truly ancient. However, carbonates are expected to be unstable on the surface of Venus today due to reaction with atmospheric sulfur compounds, and therefore any carbonates would likely have decomposed and contributed CO 2 to the greenhouse warming of the planet (Gilmore et al, 2017;Zolotov, 2007).…”

Section: Surface Weathering Reactionsmentioning

confidence: 99%

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The Inner Solar System’s Habitability Through Time

Genio¹,

Brain²,

Noack³

et al. 2005

Planetary Astrobiology

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Earth, Mars, and Venus, irradiated by an evolving Sun, have had fascinating but diverging histories of habitability. Although only Earth's surface is considered to be habitable today, all three planets might have simultaneously been habitable early in their histories. We consider how physical processes that have operated similarly or differently on these planets determined the creation and evolution of their atmospheres and surfaces over time. These include the geophysical and geochemical processes that determined the style of their interior dynamics and the presence or absence of a magnetic field; the surface-atmosphere exchange processes that acted as a source or sink for atmospheric mass and composition; the Sun-planet interactions that controlled escape of gases to space; and the atmospheric processes that interacted with these to determine climate and habitability. The divergent evolutions of the three planets provide an invaluable context for thinking about the search for life outside the Solar System.

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Solid Planet–Atmosphere Interactions

Cited by 6 publications

References 126 publications

Experiments on the reactivity of basaltic minerals and glasses in Venus surface conditions using the Glenn Extreme Environment Rig

Experiments on the reactivity of basaltic minerals and glasses in Venus surface conditions using the Glenn Extreme Environment Rig

Detectability of Remanent Magnetism in the Crust of Venus

The Inner Solar System’s Habitability Through Time

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