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    The Effect of 3D Transport-induced Disequilibrium Carbon Chemistry on the Atmospheric Structure, Phase Curves, and Emission Spectra of Hot Jupiter HD 189733b

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    Steinrueck_2019_ApJ_880_14.pdf
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    Author
    Steinrueck, Maria E.
    Parmentier, Vivien
    Showman, Adam P.
    Lothringer, Joshua D. cc
    Lupu, Roxana E.
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2019-07-18
    Keywords
    hydrodynamics
    methods: numerical
    planets and satellites: atmospheres
    planets and satellites: gaseous planets
    planets and satellites: individual (HD 189733b)
    radiative transfer
    
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    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Steinrueck, M. E., Parmentier, V., Showman, A. P., Lothringer, J. D., & Lupu, R. E. (2019). The Effect of 3D Transport-induced Disequilibrium Carbon Chemistry on the Atmospheric Structure, Phase Curves, and Emission Spectra of Hot Jupiter HD 189733b. The Astrophysical Journal, 880(1), 14.
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    Copyright © 2019. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    On hot Jupiter exoplanets, strong horizontal and vertical winds should homogenize the abundances of the important absorbers CH4 and CO much faster than chemical reactions restore chemical equilibrium. This effect, typically neglected in general circulation models (GCMs), has been suggested to explain discrepancies between observed infrared light curves and those predicted by GCMs. On the nightsides of several hot Jupiters, GCMs predict outgoing fluxes that are too large, especially in the Spitzer. 4.5 mu m band. We modified the SPARC/MITgcm to include disequilibrium abundances of CH4, CO, and H2O by assuming that the CH4/CO ratio is constant throughout the simulation domain. We ran simulations of hot Jupiter HD 189733b with eight CH4/CO ratios. In the more likely CO-dominated regime, we find temperature changes. >= 50-100 K compared to the simulation for equilibrium chemistry across large regions. This effect is large enough to affect predicted emission spectra and should thus be included in GCMs of hot Jupiters with equilibrium temperatures between 600 and 1300 K. We find that spectra in regions with strong methane absorption, including the Spitzer. 3.6 and 8 mu m bands, are strongly impacted by disequilibrium abundances. We expect chemical quenching to result in much larger nightside fluxes in the 3.6 mu m band, in stark contrast to observations. Meanwhile, we find almost no effect on predicted observations in the 4.5 mu m band, because the changes in opacity due to CO and H2O offset each other. We thus conclude that disequilibrium carbon chemistry cannot explain the observed low nightside fluxes in the 4.5 mu m band.
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/ab2598
    Version
    Final published version
    Sponsors
    NASA Origins grant [NNX12AI79G]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [80NSSC18K1248]; Heising-Simons Foundation
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab2598
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    UA Faculty Publications

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