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    Aerosol Properties of the Atmospheres of Extrasolar Giant Planets

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    Lavvas_2017_ApJ_847_32.pdf
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    Author
    Lavvas, P.
    Koskinen, T.
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2017-09-20
    Keywords
    meteorites, meteors, meteoroids
    planets and satellites: atmospheres
    planets and satellites: composition
    planets and satellites: gaseous planets
    planets and satellites: individual (HD 209458 b, HD 189733 b)
    
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    Publisher
    IOP PUBLISHING LTD
    Citation
    Aerosol Properties of the Atmospheres of Extrasolar Giant Planets 2017, 847 (1):32 The Astrophysical Journal
    Journal
    The Astrophysical Journal
    Rights
    © 2017. 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
    We use a model of aerosol microphysics to investigate the impact of high-altitude photochemical aerosols on the transmission spectra and atmospheric properties of close-in exoplanets, such as HD 209458 b and HD 189733 b. The results depend strongly on the temperature profiles in the middle and upper atmospheres, which are poorly understood. Nevertheless, our model of HD 189733 b, based on the most recently inferred temperature profiles, produces an aerosol distribution that matches the observed transmission spectrum. We argue that the hotter temperature of HD 209458 b inhibits the production of high-altitude aerosols and leads to the appearance of a clearer atmosphere than on HD 189733 b. The aerosol distribution also depends on the particle composition, photochemical production, and atmospheric mixing. Due to degeneracies among these inputs, current data cannot constrain the aerosol properties in detail. Instead, our work highlights the role of different factors in controlling the aerosol distribution that will prove useful in understanding different observations, including those from future missions. For the atmospheric mixing efficiency suggested by general circulation models, we find that the aerosol particles are small (similar to nm) and probably spherical. We further conclude that a composition based on complex hydrocarbons (soots) is the most likely candidate to survive the high temperatures in hot-Jupiter atmospheres. Such particles would have a significant impact on the energy balance of HD 189733 b's atmosphere and should be incorporated in future studies of atmospheric structure. We also evaluate the contribution of external sources to photochemical aerosol formation and find that their spectral signature is not consistent with observations.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/aa88ce
    Version
    Final published version
    Sponsors
    Programme National de Planetologie (PNP-INSU) under project AMG; Projet International de Cooperation Scientifique (PICS/CNRS) under project TAC
    Additional Links
    http://stacks.iop.org/0004-637X/847/i=1/a=32?key=crossref.2589ce51ea299b63a866617047304d82
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/aa88ce
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