Acoustic and buoyancy modes throughout stellar evolution: Seismic properties of stars at different stellar ages and masses

Parameter regions in which stars can become pulsationally unstable are found throughout the Hertzsprung‐Russell diagram. Stars of high, intermediate, low, and very low masses may cross various instability regions along their paths of evolutionary sequences. In describing them, I give special conside...

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Bibliographic Details
Published in:Astronomische Nachrichten 2012-12, Vol.333 (10), p.958-966
Main Author: Schuh, S.
Format: Article
Language:English
Subjects:
stars: evolution
stars: interiors
stars: oscillations
Sun: oscillations
waves
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Summary:Parameter regions in which stars can become pulsationally unstable are found throughout the Hertzsprung‐Russell diagram. Stars of high, intermediate, low, and very low masses may cross various instability regions along their paths of evolutionary sequences. In describing them, I give special consideration to hybrid pulsational characteristics that are particularly valuable for asteroseismic investigations, to $ \dot P $ measurements that allow us to directly follow the stellar evolutionary changes in some stars, and to new research results that stand out with respect to previous consensus (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
ISSN:0004-6337
1521-3994
DOI:10.1002/asna.201211812