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    Morphology of Hydrodynamic Winds: A Study of Planetary Winds in Stellar Environments

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    McCann_2019_ApJ_873_89.pdf
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    Author
    McCann, John
    Murray-Clay, Ruth A.
    Kratter, Kaitlin
    Krumholz, Mark R.
    Affiliation
    Univ Arizona, Dept Astron
    Univ Arizona, Steward Observ
    Issue Date
    2019-03-01
    Keywords
    hydrodynamics
    methods: numerical
    planet-star interactions
    planets and satellites: atmospheres
    planets and satellites: gaseous planets
    radiative transfer
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    John McCann et al 2019 ApJ 873 89
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 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
    Bathed in intense ionizing radiation, close-in gaseous planets undergo hydrodynamic atmospheric escape, which ejects the upper extent of their atmospheres into the interplanetary medium. Ultraviolet detections of escaping gas around transiting planets corroborate such a framework. Exposed to the stellar environment, the outflow is shaped by its interaction with the stellar wind and by the planet's orbit. We model these effects using Athena to perform 3D radiative-hydrodynamic simulations of tidally locked hydrogen atmospheres receiving large amounts of ionizing extreme-ultraviolet flux in various stellar environments for the low-magnetic-field case. Through a step-by-step exploration of orbital and stellar wind effects on the planetary outflow, we find three structurally distinct stellar wind regimes: weak, intermediate, and strong. We perform synthetic Ly alpha observations and find unique observational signatures for each regime. A weak stellar wind-which cannot confine the planetary outflow, leading to a torus of material around the star-has a pretransit, redshifted dayside arm and a slightly redward-skewed spectrum during transit. The intermediate regime truncates the dayside outflow at large distances from the planet and causes periodic disruptions of the outflow, producing observational signatures that mimic a double transit. The first of these dips is blueshifted and precedes the optical transit. Finally, strong stellar winds completely confine the outflow into a cometary tail and accelerate the outflow outward, producing large blueshifted signals posttransit. Across all three regimes, large signals occur far outside of transit, offering motivation to continue ultraviolet observations outside of direct transit.
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/ab05b8
    Version
    Final published version
    Sponsors
    National Science Foundation [AST-1411536, -1228509]; Australian Research Council [FT180100375]
    Additional Links
    http://stacks.iop.org/0004-637X/873/i=1/a=89?key=crossref.c763dd4043160f63caeb261362bf3f1d
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab05b8
    Scopus Count
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    UA Faculty Publications

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