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Stability analysis of radial oscillation modes in massive stars

Published online by Cambridge University Press:  29 August 2024

J. P. Sánchez Arias Open the ORCID record for J. P. Sánchez Arias [Opens in a new window] ,
S. Guha  and
M. Kraus Open the ORCID record for M. Kraus [Opens in a new window]
J. P. Sánchez Arias*
Affiliation:
Astronomical Institute, Czech Academy of Sciences, Fričova 298, 25165 Ondřejov, CZ
S. Guha
Affiliation:
Astronomical Institute, Czech Academy of Sciences, Fričova 298, 25165 Ondřejov, CZ Matematicko fyzikální fakulta, Univerzita Karlova, 12116 Praha, Czech Republic
M. Kraus
Affiliation:
Astronomical Institute, Czech Academy of Sciences, Fričova 298, 25165 Ondřejov, CZ
*
email: julieta.sanchez@asu.cas.cz
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Abstract

During the evolution of massive stars, their properties change significantly. But stellar parameters of massive stars have the biggest uncertainties in stellar astrophysics, specifically in the post-main sequence stages where blue supergiant stars are located. These stars experience mass loss events during their evolution which are supposed to be related to strange-modes instabilities. In this work, we explore the stability of oscillation modes in massive stars for different masses, and a range of mass-loss rates, with the aim to provide clues about the connection between strange modes instabilities and mass-loss events.

Keywords

stars: early-typestars: interiorsstars: mass loss
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 251 - 252
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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References

Gautschy, A., Glatzel, W., Gautschy, A., & Glatzel, W. 1990, MNRAS, 245, 597 Google Scholar
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