elib
DLR-Header
DLR-Logo -> http://www.dlr.de
DLR Portal Home | Imprint | Privacy Policy | Contact | Deutsch
Fontsize: [-] Text [+]

Early Habitability and Crustal Decarbonation of a Stagnant-Lid Venus

Höning, Dennis and Baumeister, Philipp and Grenfell, John Lee and Tosi, Nicola and Way, Michael J. (2021) Early Habitability and Crustal Decarbonation of a Stagnant-Lid Venus. JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS, 126 (10), e2021JE006895. Wiley. doi: 10.1029/2021JE006895. ISSN 2169-9097.

Full text not available from this repository.

Official URL: https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2021JE006895

Abstract

Little is known about the early evolution of Venus and a potential habitable period during the first 1 billion years. In particular, it remains unclear whether or not plate tectonics and an active carbonate-silicate cycle were present. In the presence of liquid water but without plate tectonics, weathering would have been limited to freshly produced basaltic crust, with an early carbon cycle restricted to the crust and atmosphere. With the evaporation of surface water, weathering would cease. With ongoing volcanism, carbonate sediments would be buried and sink downwards. Thereby, carbonates would heat up until they become unstable and the crust would become depleted in carbonates. With CO2 supply to the atmosphere the surface temperature rises further, the depth below which decarbonation occurs decreases, causing the release of even more CO2. We assess the habitable period of an early stagnant-lid Venus by employing a coupled interior-atmosphere evolution model accounting for CO2 degassing, weathering, carbonate burial, and crustal decarbonation. We find that if initial surface conditions allow for liquid water, weathering can keep the planet habitable for up to 900 Myr, followed by evaporation of water and rapid crustal carbonate depletion. For the atmospheric CO2 of stagnant-lid exoplanets, we predict a bimodal distribution, depending on whether or not these planets experienced a runaway greenhouse in their history. Planets with high atmospheric CO2 could be associated with crustal carbonate depletion as a consequence of a runaway greenhouse, whereas planets with low atmospheric CO2 would indicate active silicate weathering and thereby a habitable climate.

Item URL in elib:https://elib.dlr.de/146547/
Document Type:Article
Title:Early Habitability and Crustal Decarbonation of a Stagnant-Lid Venus
Authors:
AuthorsInstitution or Email of AuthorsAuthor's ORCID iD
Höning, DennisFree University AmsterdamUNSPECIFIED
Baumeister, PhilippPhilipp.Baumeister (at) dlr.dehttps://orcid.org/0000-0001-9284-0143
Grenfell, John LeeLee.Grenfell (at) dlr.deUNSPECIFIED
Tosi, Nicolanicola.tosi (at) dlr.deUNSPECIFIED
Way, Michael J.NASA Goddard Institute for Space Studies, New York, NY, USA; GSFC Sellers Exoplanet Environments Collaboration, Greenbelt, MD, USA; Department of Physics and Astronomy, Theoretical Astrophysics, Uppsala University, Uppsala, SwedenUNSPECIFIED
Date:17 September 2021
Journal or Publication Title:JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
Refereed publication:Yes
Open Access:Yes
Gold Open Access:No
In SCOPUS:Yes
In ISI Web of Science:Yes
Volume:126
DOI :10.1029/2021JE006895
Page Range:e2021JE006895
Publisher:Wiley
ISSN:2169-9097
Status:Published
Keywords:carbon cycle, exoplanets, habitability, planetary evolution, stagnant-lid, Venus
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 - Exploration of the Solar System
Location: Berlin-Adlershof
Institutes and Institutions:Institute of Planetary Research > Planetary Physics
Institute of Planetary Research > Extrasolar Planets and Atmospheres
Deposited By: Baumeister, Philipp
Deposited On:01 Dec 2021 09:16
Last Modified:01 Dec 2021 09:16

Repository Staff Only: item control page

Browse
Search
Help & Contact
Information
electronic library is running on EPrints 3.3.12
Copyright © 2008-2017 German Aerospace Center (DLR). All rights reserved.