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Magma Ocean, Water, and the Early Atmosphere of Venus

Salvador, Arnaud and Avice, Guillaume and Breuer, Doris and Gillmann, C. and Lammer, H and Marcq, E. and Raymond, Sean and Sakuraba, Haruka and Scherf, M and Way, MJ (2023) Magma Ocean, Water, and the Early Atmosphere of Venus. Space Science Reviews, 219 (51). Springer. doi: 10.1007/s11214-023-00995-7. ISSN 0038-6308.

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Official URL: https://link.springer.com/article/10.1007/s11214-023-00995-7


The current state and surface conditions of the Earth and its twin planet Venus are drastically different. Whether these differences are directly inherited from the earliest stages of planetary evolution, when the interior was molten, or arose later during the long-term evolution is still unclear. Yet, it is clear that water, its abundance, state, and distribution between the different planetary reservoirs, which are intimately related to the solidification and outgassing of the early magma ocean, are key components regarding past and present-day habitability, planetary evolution, and the different pathways leading to various surface conditions. In this chapter we start by reviewing the outcomes of the accretion sequence, with particular emphasis on the sources and timing of water delivery in light of available constraints, and the initial thermal state of Venus at the end of the main accretion. Then, we detail the processes at play during the early thermo-chemical evolution of molten terrestrial planets, and how they can affect the abundance and distribution of water within the different planetary reservoirs. Namely, we focus on the magma ocean cooling, solidification, and concurrent formation of the outgassed atmosphere. Accounting for the possible range of parameters for early Venus and based on the mechanisms and feedbacks described, we provide an overview of the likely evolutionary pathways leading to diverse surface conditions, from a temperate to a hellish early Venus. The implications of the resulting surface conditions and habitability are discussed in the context of the subsequent long-term interior and atmospheric evolution. Future research directions and observations are proposed to constrain the different scenarios in order to reconcile Venus’ early evolution with its current state, while deciphering which path it followed.

Item URL in elib:https://elib.dlr.de/197431/
Document Type:Article
Title:Magma Ocean, Water, and the Early Atmosphere of Venus
AuthorsInstitution or Email of AuthorsAuthor's ORCID iDORCID Put Code
Breuer, DorisUNSPECIFIEDhttps://orcid.org/0000-0001-9019-5304UNSPECIFIED
Gillmann, C.Institut für Geophysik, Department of Earth Sciences, ZürichUNSPECIFIEDUNSPECIFIED
Lammer, HSpace Research Institute, Austrian Academy of SciencesUNSPECIFIEDUNSPECIFIED
Raymond, SeanLaboratoire d’Astrophysique de Bordeaux, CNRS and Université de Bordeaux, Pessac, FranceUNSPECIFIEDUNSPECIFIED
Sakuraba, HarukaDepartment of Earth and Planetary Sciences, Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo 152-8551, JapanUNSPECIFIEDUNSPECIFIED
Scherf, MSpace Research Institute, Austrian Academy of Sciences, Graz, AustriaUNSPECIFIEDUNSPECIFIED
Way, MJNASA Goddard Institute for Space Studies, New York, NYUNSPECIFIEDUNSPECIFIED
Date:September 2023
Journal or Publication Title:Space Science Reviews
Refereed publication:Yes
Open Access:Yes
Gold Open Access:No
In ISI Web of Science:Yes
Keywords:Venus, Interior evolution, Atmosphere, Degassing
HGF - Research field:Aeronautics, Space and Transport
HGF - Program:Space
HGF - Program Themes:Space Exploration
DLR - Research area:Raumfahrt
DLR - Program:R EW - Space Exploration
DLR - Research theme (Project):R - Planetary Evolution and Life, R - Planetary Exploration
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Physics
Deposited By: Breuer, Dr. Doris
Deposited On:21 Sep 2023 08:36
Last Modified:21 Sep 2023 08:36

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