Solid Planet–Atmosphere Interactions

Zolotov, M. Yu.

doi:10.1016/b978-0-444-53802-4.00182-2

Cited by 5 publications

(4 citation statements)

References 155 publications

(183 reference statements)

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“…Our work confirms that glass phases are highly reactive under Venus surface conditions, as hypothesized and suggested by earlier research (i.e., Berger et al., 2019; Frenkel & Zabalueva, 1983; Zolotov, 2015). High cation mobility within basaltic glasses relative to basaltic minerals was demonstrated in experiments by Treiman and Allen (1994), who exposed crushed lunar basaltic simulant glass to pure CO 2 at 750 °C for 5 days.…”

Section: Discussionsupporting

confidence: 92%

“…The formation of these phases is further suggested by the oxygen fugacity models by Semprich et al. (2020) and suggested in other studies, but not observed on our samples (Berger et al., 2019; Fegley et al., 1992; Gilmore et al., 2017; Yu, 2007; 2018; Zolotov, 2015, 2018).…”

Section: Discussionsupporting

confidence: 87%

“…Our modeling suggested the stability of orthopyroxene (enstatite MgSiO 3 ) and quartz (SiO 2 ), with some of the original diopside and augite still being present after equilibrium was reached; effectively FactSage is suggesting partial removal of mobile Ca components from the pyroxenes under Venus surface conditions, akin to the allochemical re-equilibration during low-grade metamorphism (Table 3). The formation of these phases is further suggested by the oxygen fugacity models by Semprich et al (2020) and suggested in other studies, but not observed on our samples (Berger et al, 2019;Fegley et al, 1992;Gilmore et al, 2017;Yu, 2007;Zolotov, 2015Zolotov, , 2018.…”

Section: Pyroxenes (Augite and Diopside)supporting

confidence: 69%

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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: Discussionsupporting

confidence: 92%

Section: Discussionsupporting

confidence: 87%

Section: Pyroxenes (Augite and Diopside)supporting

confidence: 69%

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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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