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Quantification of the environment of cool stars using numerical simulations

Published online by Cambridge University Press:  16 August 2023

J. J. Chebly Open the ORCID record for J. J. Chebly [Opens in a new window] ,
Julián D. Alvarado-Gómez  and
Katja Poppenhaeger
J. J. Chebly
Affiliation:
Leibniz Institute for Astrophysics, An der Sternwarte 16, 14482, Potsdam, Germany Institute of Physics and Astronomy, University of Potsdam, Potsdam-Golm, 14476, Germany
Julián D. Alvarado-Gómez
Affiliation:
Leibniz Institute for Astrophysics, An der Sternwarte 16, 14482, Potsdam, Germany
Katja Poppenhaeger
Affiliation:
Leibniz Institute for Astrophysics, An der Sternwarte 16, 14482, Potsdam, Germany Institute of Physics and Astronomy, University of Potsdam, Potsdam-Golm, 14476, Germany
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Abstract

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Stars interact with their planets through gravitation, radiation, and magnetic fields. Although magnetic activity decreases with time, reducing associated high-energy (e.g., coronal XUV emission, flares), stellar winds persist throughout the entire evolution of the system. Their cumulative effect will be dominant for both the star and for possible orbiting exoplanets, affecting in this way the expected habitability conditions. However, observations of stellar winds in low-mass main sequence stars are limited, which motivates the usage of models as a pathway to explore how these winds look like and how they behave. Here we present the results from a grid of 3D state-of-the-art stellar wind models for cool stars (spectral types F to M). We explore the role played by the different stellar properties (mass, radius, rotation, magnetic field) on the characteristics of the resulting magnetized winds (mass and angular momentum losses, terminal speeds, wind topology) and isolate the most important dependencies between the parameters involved. These results will be used to establish scaling laws that will complement the lack of stellar wind observational constraints.

Keywords

Stars: low-massstars: magnetic fieldsstars: mass lossstars: windsoutflowsmethods: numericalmagnetic fields (magnetohydrodynamics:) MHD
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 185 - 190
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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