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The atmospheres of rocky exoplanets : II. Influence of surface composition on the diversity of cloud condensates

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Date
02/2022
Author
Herbort, O.
Woitke, P.
Helling, C.
Zerkle, A.L.
Funder
European Commission
Grant ID
860470
Keywords
Planets and satellites: Atmospheres
Planets and satellites: composition
Planets and satellites: Surfaces
Planets and satellites: terrestrial planets
Astrochemistry
QB Astronomy
QC Physics
QD Chemistry
I-PW
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Abstract
Clouds are an integral part of planetary atmospheres, with most planets hosting clouds. Understanding not only the formation, but also the composition of clouds, is crucial to understand future observations. As observations of the planet's surface will remain very difficult, it is essential to link the observable high atmosphere gas and cloud composition to the surface conditions. We present a fast and simple chemical equilibrium model for the troposphere of rocky exoplanets, which is in chemical and phase equilibrium with the crust. The hydrostatic equilibrium atmosphere is built from bottom to top. In each atmospheric layer, chemical equilibrium is solved and all thermally stable condensates are removed, depleting the atmosphere above in the effected elements. These removed condensates build an upper limit for cloud formation and can be separated into high and low temperature condensates. The most important cloud condensates for 1000K >∼ Tgas >∼ 400K are KCl[s], NaCl[s], FeS[s], FeS2[s], FeO[s], Fe2O3[s], and Fe3O4[s]. For Tgas ∼< 400K H2O[l,s], C[s], NH3[s], NH4Cl[s], and NH4SH[s] are thermally stable, while for even lower temperatures of Tgas ≤ 150K CO2[s], CH4[s], NH3[s], and H2S[s] become stable. The inclusion of clouds with trace abundances results in the thermal stability of a total of 72 condensates for atmospheres with different surface conditions (300K ≤ Tsurf ≤ 1000K and psurf = 1 bar; 100 bar). The different cloud condensates are not independent of each other, but follow sequences of condensation, which are robust against changes in crust composition, surface pressure, and surface temperature. Independent of the existence of water as a crust condensate, H2O[l,s] is a thermally stable cloud condensate for all investigated elemental abundances. However, the water cloud base depends on the hydration level of the crust. Therefore, the detection of water condensates alone does not necessarily imply stable water on the surface, even if the temperature could allow for water condensation.
Citation
Herbort , O , Woitke , P , Helling , C & Zerkle , A L 2022 , ' The atmospheres of rocky exoplanets : II. Influence of surface composition on the diversity of cloud condensates ' , Astronomy and Astrophysics , vol. 658 , A180 . https://doi.org/10.1051/0004-6361/202141636
Publication
Astronomy and Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/202141636
ISSN
0004-6361
Type
Journal article
Rights
Copyright © ESO 2022. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1051/0004-6361/202141636.
Description
O.H. acknowledges the PhD stipend form the University of St Andrews’ Centre for Exoplanet Science. P.W. and Ch.H. acknowledge funding from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON).
Collections
  • University of St Andrews Research
URL
https://arxiv.org/abs/2111.14144
URI
http://hdl.handle.net/10023/25041

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