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    UV Exoplanet Transmission Spectral Features as Probes of Metals and Rainout

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    Lothringer_2020_ApJL_898_L14.pdf
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    Author
    Lothringer, Joshua D. cc
    Fu, Guangwei
    Sing, David K.
    Barman, Travis S. cc
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2020-07
    Keywords
    Exoplanet atmospheres
    Hot Jupiters
    Exoplanets
    Extrasolar gas giants
    Near ultraviolet astronomy
    Transmission spectroscopy
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Joshua D. Lothringer et al 2020 ApJL 898 L14
    Journal
    ASTROPHYSICAL JOURNAL LETTERS
    Rights
    Copyright © 2020. 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
    The transmission spectra of ultra-hot Jupiters observed shortward of 0.5 mu m indicate strong absorption. Previous explanations have included scattering, photochemistry, escaping metals, and disequilibrium chemistry. In this Letter, we show that slopes and features shortward of 0.5 mu m can be caused by opacity not commonly considered in atmosphere models of exoplanets but guaranteed to be present if conditions are near chemical equilibrium including, but not limited to, atoms and ions of Fe, Ti, Ni, Ca, Cr, Mn, and SiO. Using the PHOENIX atmosphere model, we describe how the short-wavelength transit spectrum varies with equilibrium temperature between 1000 K and 4000 K, as well as the effect that the rainout of condensates has at these wavelengths. We define two spectral indices to quantify the strength of the NUV and blue absorption compared to that in the red-optical, finding that the NUV transit depth will significantly exceed the transit depth from Rayleigh scattering alone for all hot Jupiters down to around 1000 K. In the blue-optical, hot Jupiters warmer than 2000 K will have transit depths larger than that from Rayleigh scattering, but below 2000 K, Rayleigh scattering can dominate, if present. We further show that these spectral indices may be used to trace the effects of rainout. We then compare our simulated transit spectra to existing observations of WASP-12b, WASP-33b, WASP-76b, and WASP-121b. Further observation of exoplanets at these wavelengths should be prioritized in the coming years as the Hubble Space Telescope nears the end of its operational capability.
    Note
    Immediate access
    ISSN
    2041-8205
    EISSN
    2041-8213
    DOI
    10.3847/2041-8213/aba265
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/2041-8213/aba265
    Scopus Count
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    UA Faculty Publications

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