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  The Habitability of Venus

Westall, F., Höning, D., Avice, G., Gentry, D., Gerya, T., Gillmann, C., Izenberg, N., Way, M. J., Wilson, C. (2023): The Habitability of Venus. - Space Science Reviews, 219, 17.
https://doi.org/10.1007/s11214-023-00960-4

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 Creators:
Westall, F.1, Author
Höning, Dennis2, Author              
Avice, G.1, Author
Gentry, D.1, Author
Gerya, T.1, Author
Gillmann, C.1, Author
Izenberg, N.1, Author
Way, M. J.1, Author
Wilson, C.1, Author
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1External Organizations, ou_persistent22              
2Potsdam Institute for Climate Impact Research, Potsdam, ou_persistent13              

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 Abstract: 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 ), 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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Language(s): eng - English
 Dates: 2023-02-222023-02-22
 Publication Status: Finally published
 Pages: 53
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1007/s11214-023-00960-4
PIKDOMAIN: RD1 - Earth System Analysis
Organisational keyword: RD1 - Earth System Analysis
MDB-ID: pending
OATYPE: Hybrid - DEAL Springer Nature
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Title: Space Science Reviews
Source Genre: Journal, SCI, Scopus, p3
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Pages: - Volume / Issue: 219 Sequence Number: 17 Start / End Page: - Identifier: CoNE: https://publications.pik-potsdam.de/cone/journals/resource/journals458
Publisher: Springer