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Title: Photoevaporative flows from exoplanet atmospheres: a 3D radiative hydrodynamic parameter study

Abstract

he photoionization-driven evaporation of planetary atmospheres has emerged as a potentially fundamental process for planets on short-period orbits. While 1D studies have proven the effectiveness of stellar fluxes at altering the atmospheric mass and composition for sub-Jupiter mass planets, there remains much that is uncertain with regard to the larger scale, multidimensional nature of such ‘planetary wind’ flows. In this paper we use a new radiation-hydrodynamic platform to simulate atmospheric evaporative flows. Using the astrobear adaptive mesh refinement (amr) multiphysics code in a co-rotating frame centred on the planet, we model the transfer of ionizing photons into the atmosphere, the subsequent launch of the wind and the wind’s large-scale evolution subject to tidal and non-inertial forces. We run simulations for planets of 0.263 and 0.07 Jupiter masses and stellar fluxes of 2 × 1013 and 2 × 1014 photons cm-2 s-1. Our results reveal new, potentially observable planetary wind flow patterns, including the development, in some cases, of an extended neutral tail lagging behind the planet in its orbit.

Authors:
ORCiD logo [1];  [1];  [1];  [2];  [3];  [1]
  1. Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA
  2. Department of Physics, University of California, Santa Barbara, CA 93106, USA
  3. Physics and Astronomy Department, University of California, Santa Cruz, CA 95064, USA
Publication Date:
Research Org.:
Univ. of Rochester, NY (United States)
Sponsoring Org.:
USDOE Office of Energy Efficiency and Renewable Energy (EERE), Renewable Power Office. Wind Energy Technologies Office; National Science Foundation (NSF); Space Telescope Science Institute
OSTI Identifier:
1485345
Alternate Identifier(s):
OSTI ID: 1610512
Grant/Contract Number:  
SC0001063; TG-AST120060; ACI-1548562; AST-1515648; AST-1411536; HST-AR-12832.01-A
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 483 Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United Kingdom
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; hydrodynamics; planets and satellites; atmospheres; planet-star interactions

Citation Formats

Debrecht, Alex, Carroll-Nellenback, Jonathan, Frank, Adam, McCann, John, Murray-Clay, Ruth, and Blackman, Eric G. Photoevaporative flows from exoplanet atmospheres: a 3D radiative hydrodynamic parameter study. United Kingdom: N. p., 2018. Web. doi:10.1093/mnras/sty3212.
Debrecht, Alex, Carroll-Nellenback, Jonathan, Frank, Adam, McCann, John, Murray-Clay, Ruth, & Blackman, Eric G. Photoevaporative flows from exoplanet atmospheres: a 3D radiative hydrodynamic parameter study. United Kingdom. doi:https://doi.org/10.1093/mnras/sty3212
Debrecht, Alex, Carroll-Nellenback, Jonathan, Frank, Adam, McCann, John, Murray-Clay, Ruth, and Blackman, Eric G. Tue . "Photoevaporative flows from exoplanet atmospheres: a 3D radiative hydrodynamic parameter study". United Kingdom. doi:https://doi.org/10.1093/mnras/sty3212.
@article{osti_1485345,
title = {Photoevaporative flows from exoplanet atmospheres: a 3D radiative hydrodynamic parameter study},
author = {Debrecht, Alex and Carroll-Nellenback, Jonathan and Frank, Adam and McCann, John and Murray-Clay, Ruth and Blackman, Eric G.},
abstractNote = {he photoionization-driven evaporation of planetary atmospheres has emerged as a potentially fundamental process for planets on short-period orbits. While 1D studies have proven the effectiveness of stellar fluxes at altering the atmospheric mass and composition for sub-Jupiter mass planets, there remains much that is uncertain with regard to the larger scale, multidimensional nature of such ‘planetary wind’ flows. In this paper we use a new radiation-hydrodynamic platform to simulate atmospheric evaporative flows. Using the astrobear adaptive mesh refinement (amr) multiphysics code in a co-rotating frame centred on the planet, we model the transfer of ionizing photons into the atmosphere, the subsequent launch of the wind and the wind’s large-scale evolution subject to tidal and non-inertial forces. We run simulations for planets of 0.263 and 0.07 Jupiter masses and stellar fluxes of 2 × 1013 and 2 × 1014 photons cm-2 s-1. Our results reveal new, potentially observable planetary wind flow patterns, including the development, in some cases, of an extended neutral tail lagging behind the planet in its orbit.},
doi = {10.1093/mnras/sty3212},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 483,
place = {United Kingdom},
year = {2018},
month = {11}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
DOI: https://doi.org/10.1093/mnras/sty3212

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Cited by: 3 works
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