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Title: Stellar influence on heavy ion escape from unmagnetized exoplanets

Abstract

Abstract Planetary habitability is in part determined by the atmospheric evolution of a planet; one key component of such evolution is escape of heavy ions to space. Ion-loss processes are sensitive to the plasma environment of the planet, dictated by the stellar wind and stellar radiation. These conditions are likely to vary from what we observe in our own Solar system when considering a planet in the habitable zone around an M-dwarf. Here, we use a hybrid global plasma model to perform a systematic study of the changing plasma environment and ion escape as a function of stellar input conditions, which are designed to mimic those of potentially habitable planets orbiting M-dwarfs. We begin with a nominal case of a solar wind experienced at Mars today, and incrementally modify the interplanetary magnetic field orientation and strength, dynamic pressure, and Extreme Ultraviolet input. We find that both ion-loss morphology and overall rates vary significantly, and in cases where the stellar wind pressure was increased, the ion loss began to be diffusion or production limited with roughly half of all produced ions being lost. This limit implies that extreme care must be taken when extrapolating loss processes observed in the Solar systemmore » to extreme environments.« less

Authors:
ORCiD logo [1];  [2];  [1]
  1. Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA
  2. Department of Electronics and Nanoengineering, School of Electrical Engineering, Aalto University, Espoo, Finland, Finnish Meteorological Institute, Helsinki, Finland
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1507209
Alternate Identifier(s):
OSTI ID: 1577640
Grant/Contract Number:  
AC02-05CH11231
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: 486 Journal Issue: 1; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics; methods: numerical; planets and satellites: atmospheres; planet–star interactions; planetary systems

Citation Formats

Egan, Hilary, Jarvinen, Riku, and Brain, David. Stellar influence on heavy ion escape from unmagnetized exoplanets. United Kingdom: N. p., 2019. Web. https://doi.org/10.1093/mnras/stz788.
Egan, Hilary, Jarvinen, Riku, & Brain, David. Stellar influence on heavy ion escape from unmagnetized exoplanets. United Kingdom. https://doi.org/10.1093/mnras/stz788
Egan, Hilary, Jarvinen, Riku, and Brain, David. Fri . "Stellar influence on heavy ion escape from unmagnetized exoplanets". United Kingdom. https://doi.org/10.1093/mnras/stz788.
@article{osti_1507209,
title = {Stellar influence on heavy ion escape from unmagnetized exoplanets},
author = {Egan, Hilary and Jarvinen, Riku and Brain, David},
abstractNote = {Abstract Planetary habitability is in part determined by the atmospheric evolution of a planet; one key component of such evolution is escape of heavy ions to space. Ion-loss processes are sensitive to the plasma environment of the planet, dictated by the stellar wind and stellar radiation. These conditions are likely to vary from what we observe in our own Solar system when considering a planet in the habitable zone around an M-dwarf. Here, we use a hybrid global plasma model to perform a systematic study of the changing plasma environment and ion escape as a function of stellar input conditions, which are designed to mimic those of potentially habitable planets orbiting M-dwarfs. We begin with a nominal case of a solar wind experienced at Mars today, and incrementally modify the interplanetary magnetic field orientation and strength, dynamic pressure, and Extreme Ultraviolet input. We find that both ion-loss morphology and overall rates vary significantly, and in cases where the stellar wind pressure was increased, the ion loss began to be diffusion or production limited with roughly half of all produced ions being lost. This limit implies that extreme care must be taken when extrapolating loss processes observed in the Solar system to extreme environments.},
doi = {10.1093/mnras/stz788},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 486,
place = {United Kingdom},
year = {2019},
month = {3}
}

Journal Article:
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https://doi.org/10.1093/mnras/stz788

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