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Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b II. Mapping the effects of gas kinetics

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Helling_2020_AA_Understanding_VoR_CCBY.pdf (46.18Mb)
Date
03/2020
Author
Molaverdikhani, K.
Helling, Ch.
Lew, B. W. P.
MacDonald, R. J.
Samra, D.
Iro, N.
Woitke, P.
Parmentier, V.
Keywords
Planets and satellites: atmospheres
Planets and satellites: gaseous planets
Planets and satellites: composition
Planets and satellites: individual: ultra-hot jupiters
Astrochemistry
QB Astronomy
QC Physics
QD Chemistry
Astronomy and Astrophysics
Space and Planetary Science
T-NDAS
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Abstract
Aims. The atmospheres of ultra-hot Jupiters (UHJs) are commonly considered to be at thermochemical equilibrium. We aim to provide disequilibrium chemistry maps for a global understanding of the chemistry in the atmosphere of HAT-P-7b and assess the importance of disequilibrium chemistry on UHJs. Methods. We applied a hierarchical modeling approach using 97 1D atmospheric profiles from a 3D general circulation model of HAT-P-7b. For each atmospheric 1D profile, we evaluated our kinetic cloud formation model consistently with the local gas-phase composition in chemical equilibrium. This served as input to study the quenching of dominating CHNO-binding molecules. We evaluated quenching results from a zeroth-order approximation in comparison to a kinetic gas-phase approach. Results. We find that the zeroth-order approach of estimating quenching points agrees well with the full gas-kinetic modeling results. However, it underestimates the quenching levels by about one order of magnitude at high temperatures. Chemical disequilibrium has the greatest effect on the nightside and morning abundance of species such as H, H2O, CH4, CO2, HCN, and all CnHm molecules; heavier CnHm molecules are more affected by disequilibrium processes. The CO abundance, however, is affected only marginally. While dayside abundances also notably change, those around the evening terminator of HAT-P-7b are the least affected by disequilibrium processes. The latter finding may partially explain the consistency of observed transmission spectra of UHJs with atmospheres in thermochemical equilibrium. Photochemistry only negligibly affects molecular abundances and quenching levels. Conclusions. In general, the quenching points of the atmosphere of HAT-P-7b are at much lower pressures than in the cooler hot-jupiters. We propose several avenues to determining the effect of disequilibrium processes on UHJs that are in general based on abundance and opacity measurements at different local times. It remains a challenge to completely disentangle this from the chemical effects of clouds and that of a primordial nonsolar abundance.
Citation
Molaverdikhani , K , Helling , C , Lew , B W P , MacDonald , R J , Samra , D , Iro , N , Woitke , P & Parmentier , V 2020 , ' Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b II. Mapping the effects of gas kinetics ' , Astronomy & Astrophysics , vol. 635 , A31 . https://doi.org/10.1051/0004-6361/201937044
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201937044
ISSN
0004-6361
Type
Journal article
Rights
Copyright © K. Molaverdikhani et al. 2020. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Description
Funding: Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1.
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  • University of St Andrews Research
URI
http://hdl.handle.net/10023/19707

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