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    A New Model of Roche Lobe Overflow for Short-period Gaseous Planets and Binary Stars

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    Author
    Jackson, Brian cc
    Arras, Phil
    Penev, K. cc
    Peacock, Sarah cc
    Marchant, Pablo cc
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2017-01-24
    Keywords
    binaries: close
    planet-star interactions
    planets and satellites: gaseous planets
    planets and satellites: individual (CoRoT-24 b, WASP-12 b, PTFO8-8695)
    
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    Publisher
    IOP PUBLISHING LTD
    Citation
    A New Model of Roche Lobe Overflow for Short-period Gaseous Planets and Binary Stars 2017, 835 (2):145 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
    Some close-in gaseous exoplanets are nearly in Roche lobe contact, and previous studies show that tidal decay can drive hot Jupiters into contact during the main sequence of their host stars. Improving on a previous model, we present a revised model for mass transfer in a semidetached binary system that incorporates an extended atmosphere around the donor and allows for an arbitrary mass ratio. We apply this new formalism to hypothetical, confirmed, and candidate planetary systems to estimate mass-loss rates and compare with models of evaporative mass loss. Overflow may be significant for hot Neptunes out to periods of similar to 2 days, while for hot Jupiters, it may only be important inward of 0.5 days. We find that CoRoT-24 b may be losing mass at a rate of more than an Earth mass in a gigayear. The hot Jupiter WASP-12 b may lose an Earth mass in a megayear, while the putative planet PTFO8-8695 orbiting a T Tauri star might shed its atmosphere in a few megayears. We point out that the orbital expansion that can accompany mass transfer may be less effective than previously considered because the gas accreted by the host star removes some of the angular momentum from the orbit, but simple scaling arguments suggest that the Roche lobe overflow might remain stable. Consequently, the recently discovered small planets in ultrashort periods (< 1 day) may not be the remnants of hot Jupiters/Neptunes. The new model presented here has been incorporated into Modules for Experiments in Stellar Astrophysics (MESA).
    ISSN
    1538-4357
    DOI
    10.3847/1538-4357/835/2/145
    Version
    Final published version
    Sponsors
    NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; NASA Grant [NNX13AQ62G]; NASA Origins Grant [NNX14AE16G]; NASA ATP grant [NNH12ZDA]
    Additional Links
    http://stacks.iop.org/0004-637X/835/i=2/a=145?key=crossref.94358715f8518a0780c563b3d8206c5e
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/835/2/145
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    UA Faculty Publications

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