dc.contributor.author
Barth, Patrick
dc.contributor.author
Carone, Ludmila
dc.contributor.author
Barnes, Rory
dc.contributor.author
Noack, Lena
dc.contributor.author
Molliere, Paul
dc.contributor.author
Henning, Thomas
dc.date.accessioned
2021-12-01T14:04:44Z
dc.date.available
2021-12-01T14:04:44Z
dc.identifier.uri
https://refubium.fu-berlin.de/handle/fub188/31881
dc.identifier.uri
http://dx.doi.org/10.17169/refubium-31613
dc.description.abstract
Recent observations of the potentially habitable planets TRAPPIST-1 e, f, and g suggest that they possess large water mass fractions of possibly several tens of weight percent of water, even though the host star's activity should drive rapid atmospheric escape. These processes can photolyze water, generating free oxygen and possibly desiccating the planet. After the planets formed, their mantles were likely completely molten with volatiles dissolving and exsolving from the melt. To understand these planets and prepare for future observations, the magma ocean phase of these worlds must be understood. To simulate these planets, we have combined existing models of stellar evolution, atmospheric escape, tidal heating, radiogenic heating, magma-ocean cooling, planetary radiation, and water-oxygen-iron geochemistry. We present , a versatile magma-ocean evolution model, validated against the rocky super-Earth GJ 1132b and early Earth. We simulate the coupled magma-ocean atmospheric evolution of TRAPPIST-1 e, f, and g for a range of tidal and radiogenic heating rates, as well as initial water contents between 1 and 100 Earth oceans. We also reanalyze the structures of these planets and find they have water mass fractions of 0–0.23, 0.01–0.21, and 0.11–0.24 for planets e, f, and g, respectively. Our model does not make a strong prediction about the water and oxygen content of the atmosphere of TRAPPIST-1 e at the time of mantle solidification. In contrast, the model predicts that TRAPPIST-1 f and g would have a thick steam atmosphere with a small amount of oxygen at that stage. For all planets that we investigated, we find that only 3–5% of the initial water will be locked in the mantle after the magma ocean solidified.
en
dc.format.extent
25 Seiten
dc.rights.uri
https://creativecommons.org/licenses/by/4.0/
dc.subject
Terrestrial planets
en
dc.subject
Planetary atmospheres
en
dc.subject
Magma oceans
en
dc.subject.ddc
500 Naturwissenschaften und Mathematik::520 Astronomie::520 Astronomie und zugeordnete Wissenschaften
dc.title
Magma Ocean Evolution of the TRAPPIST-1 Planets
dc.type
Wissenschaftlicher Artikel
dcterms.bibliographicCitation.doi
10.1089/ast.2020.2277
dcterms.bibliographicCitation.journaltitle
Astrobiology
dcterms.bibliographicCitation.number
11
dcterms.bibliographicCitation.pagestart
1325
dcterms.bibliographicCitation.pageend
1349
dcterms.bibliographicCitation.volume
21
dcterms.bibliographicCitation.url
https://doi.org/10.1089/ast.2020.2277
refubium.affiliation
Geowissenschaften
refubium.affiliation.other
Institut für Geologische Wissenschaften / Fachrichtung Geochemie, Hydrogeologie, Mineralogie
refubium.resourceType.isindependentpub
no
dcterms.accessRights.openaire
open access
dcterms.isPartOf.eissn
1557-8070
refubium.resourceType.provider
WoS-Alert