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Title: Effects of radiation pressure on the evaporative wind of HD 209458b

Abstract

ABSTRACT The role of radiation pressure in shaping exoplanet photoevaporation remains a topic of contention. Radiation pressure from the exoplanet’s host star has been proposed as a mechanism to drive the escaping atmosphere into a ‘cometary’ tail and explain the high velocities observed in systems where mass-loss is occurring. In this paper, we present results from high-resolution 3D hydrodynamic simulations of a planet similar to HD 209458b. We self-consistently launch a wind flowing outwards from the planet by calculating the ionization and heating resulting from incident high-energy radiation, and account for radiation pressure. We first present a simplified calculation, setting a limit on the Lyman-α flux required to drive the photoevaporated planetary material to larger radii and line-of-sight velocities. We then present the results of our simulations, which confirm the limits determined by our analytic calculation. We thus demonstrate that, within the limits of our hydrodynamic simulation and for the Lyman-α fluxes expected for HD 209458, radiation pressure is unlikely to significantly affect photoevaporative winds or to explain the high velocities at which wind material is observed, though further possibilities remain to be investigated.

Authors:
ORCiD logo [1];  [1];  [1]; ORCiD logo [1];  [2];  [3];  [4]
  1. Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA
  2. Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, A-8042 Graz, Austria
  3. Department of Physics, University of California, Santa Barbara, CA 93106, USA
  4. Physics and Astronomy Department, University of California, Santa Cruz, CA 95064, USA
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1601507
Grant/Contract Number:  
[SC0001063]
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: 493 Journal Issue: 1]; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English

Citation Formats

Debrecht, Alex, Carroll-Nellenback, Jonathan, Frank, Adam, Blackman, Eric G., Fossati, Luca, McCann, John, and Murray-Clay, Ruth. Effects of radiation pressure on the evaporative wind of HD 209458b. United Kingdom: N. p., 2020. Web. doi:10.1093/mnras/staa351.
Debrecht, Alex, Carroll-Nellenback, Jonathan, Frank, Adam, Blackman, Eric G., Fossati, Luca, McCann, John, & Murray-Clay, Ruth. Effects of radiation pressure on the evaporative wind of HD 209458b. United Kingdom. doi:10.1093/mnras/staa351.
Debrecht, Alex, Carroll-Nellenback, Jonathan, Frank, Adam, Blackman, Eric G., Fossati, Luca, McCann, John, and Murray-Clay, Ruth. Thu . "Effects of radiation pressure on the evaporative wind of HD 209458b". United Kingdom. doi:10.1093/mnras/staa351.
@article{osti_1601507,
title = {Effects of radiation pressure on the evaporative wind of HD 209458b},
author = {Debrecht, Alex and Carroll-Nellenback, Jonathan and Frank, Adam and Blackman, Eric G. and Fossati, Luca and McCann, John and Murray-Clay, Ruth},
abstractNote = {ABSTRACT The role of radiation pressure in shaping exoplanet photoevaporation remains a topic of contention. Radiation pressure from the exoplanet’s host star has been proposed as a mechanism to drive the escaping atmosphere into a ‘cometary’ tail and explain the high velocities observed in systems where mass-loss is occurring. In this paper, we present results from high-resolution 3D hydrodynamic simulations of a planet similar to HD 209458b. We self-consistently launch a wind flowing outwards from the planet by calculating the ionization and heating resulting from incident high-energy radiation, and account for radiation pressure. We first present a simplified calculation, setting a limit on the Lyman-α flux required to drive the photoevaporated planetary material to larger radii and line-of-sight velocities. We then present the results of our simulations, which confirm the limits determined by our analytic calculation. We thus demonstrate that, within the limits of our hydrodynamic simulation and for the Lyman-α fluxes expected for HD 209458, radiation pressure is unlikely to significantly affect photoevaporative winds or to explain the high velocities at which wind material is observed, though further possibilities remain to be investigated.},
doi = {10.1093/mnras/staa351},
journal = {Monthly Notices of the Royal Astronomical Society},
number = [1],
volume = [493],
place = {United Kingdom},
year = {2020},
month = {2}
}

Journal Article:
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DOI: 10.1093/mnras/staa351

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