The modeling of Venus' degassing in terms of K-Ar system

Volkov, V. P.; Frenkel, M. Ya.

doi:10.1007/bf00572140

Cited by 13 publications

(5 citation statements)

References 13 publications

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“…Numerical values are in line with the lower estimates by Fegley and Prinn [] or Bullock and Grinspoon [] but remain too low compared to their upper range (up to 11 km 3 /yr for the former and 9.2 km 3 /yr for the latter). Volcanic production rates since the last major event are in line with past estimates [ Volkov and Frenkel , ; Matsui and Tajika , ; Bullock et al ., , ; Strom et al ., ; Price and Suppe , ]. For comparison, a list of the main simulations is shown on Table .…”

Section: Resultssupporting

confidence: 88%

Atmosphere/mantle coupling and feedbacks on Venus

2014

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We investigate the coupled evolution of the atmosphere and mantle on Venus. Here we focus on mechanisms that deplete or replenish the atmosphere: atmospheric escape to space and volcanic degassing of the mantle. These processes are linked to obtain a coupled model of mantle convection and atmospheric evolution, including feedback of the atmosphere on the mantle via the surface temperature. During early atmospheric evolution, hydrodynamic escape is dominant, while for later evolution we focus on nonthermal escape, as observed by the Analyzer of Space Plasma and Energetic Atoms instrument on the Venus Express Mission. The atmosphere is replenished by volcanic degassing from the mantle, using mantle convection simulations based on those of Armann and Tackley [2012], and include episodic lithospheric overturn. The evolving surface temperature is calculated from the amount of CO 2 and water in the atmosphere using a gray radiative-convective atmosphere model. This surface temperature in turn acts as a boundary condition for the mantle convection model. We obtain a Venus-like behavior (episodic lid) for the solid planet and an atmospheric evolution leading to the present conditions. CO 2 pressure is unlikely to vary much over the history of the planet, with only a 0.25-20% postmagma-ocean buildup. In contrast, atmospheric water vapor pressure is strongly sensitive to volcanic activity, leading to variations in surface temperatures of up to 200 K, which have an effect on volcanic activity and mantle convection. Low surface temperatures trigger a mobile lid regime that stops once surface temperatures rise again, making way to stagnant lid convection that insulates the mantle.

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Section: Resultssupporting

confidence: 88%

Atmosphere/mantle coupling and feedbacks on Venus

2014

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“…K, U, and Th in Venus' rocks were measured by five Venera and Vega probes (Surkov et al, 1987a), and their abundances in Venus' interior were discussed by Pollack and Black (1982), Volkov and Frenkel (1993), Paper II, Namiki and Solomon (1998), and Kaula (1999). We conclude from these papers that the abundances for Venus may be similar to those for the Earth.…”

Section: Production Of Helium On Venusmentioning

confidence: 92%

Helium on Mars and Venus: EUVE observations and modeling

Krasnopolsky

Gladstone

2005

Icarus

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“…It has therefore been postulated that one could infer the tectonic style of a planet based on its volatile history and atmosphere characteristics. In particular, Venus' 40 Ar measurements have been used to suggest that the planet only outgassed 10 to 34% of its total 40 Ar inventory (Kaula 1999;O'Rourke and Korenaga 2015;Namiki and Solomon 1998;Volkov and Frenkel 1993), compared to Earth's 50%. That would imply Venus outgassing was limited during most of its evolution or was only important during its early history (when 40 Ar had not formed yet).…”

Section: Tectonicsmentioning

confidence: 99%

The Habitability of Venus

et al. 2023

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Venus today is inhospitable at the surface, its average temperature of 750 K being incompatible to the existence of life as we know it. However, the potential for past surface habitability and upper atmosphere (cloud) habitability at the present day is hotly debated, as the ongoing discussion regarding a possible phosphine signature coming from the clouds shows. We review current understanding about the evolution of Venus with special attention to scenarios where the planet may have been capable of hosting microbial life. We compare the possibility of past habitability on Venus to the case of Earth by reviewing the various hypotheses put forth concerning the origin of habitable conditions and the emergence and evolution of plate tectonics on both planets. Life emerged on Earth during the Hadean when the planet was dominated by higher mantle temperatures (by about $200~^{\circ}\text{C}$ 200 ∘ C ), an uncertain tectonic regime that likely included squishy lid/plume-lid and plate tectonics, and proto continents. Despite the lack of well-preserved crust dating from the Hadean and Paleoarchean, we attempt to review current understanding of the environmental conditions during this critical period based on zircon crystals and geochemical signatures from this period, as well as studies of younger, relatively well-preserved rocks from the Paleoarchean. For these early, primitive life forms, the tectonic regime was not critical but it became an important means of nutrient recycling, with possible consequences on the global environment in the long-term, that was essential to the continuation of habitability and the evolution of life. For early Venus, the question of stable surface water is closely related to tectonics. We discuss potential transitions between stagnant lid and (episodic) tectonics with crustal recycling, as well as consequences for volatile cycling between Venus’ interior and atmosphere. In particular, we review insights into Venus’ early climate and examine critical questions about early rotation speed, reflective clouds, and silicate weathering, and summarize implications for Venus’ long-term habitability. Finally, the state of knowledge of the Venusian clouds and the proposed detection of phosphine is covered.

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The modeling of Venus' degassing in terms of K-Ar system

Cited by 13 publications

References 13 publications

Atmosphere/mantle coupling and feedbacks on Venus

Atmosphere/mantle coupling and feedbacks on Venus

Helium on Mars and Venus: EUVE observations and modeling

The Habitability of Venus

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