Abstract
Thermal overstability of non-radial eigenmodes of stars is discussed as one of possible causes for generating non-thermal motions in the stellar atmosphere. The nature of oscillatory motions in stars is first considered both in the local and the global stand points. Then, the excitation of eigen-oscillations is discussed and results of numerical studies so far made are reviewed for the vibrational stability of various stellar models against non-radial oscillations. It is found that many of nonradial p-modes of high tesseral harmonics are likely excited in various stars of the HR diagram and that they possibly manifest themselves as non-thermal velocity fields in the stellar atmosphere.
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© 1980 Springer-Verlag
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Osaki, Y. (1980). Generation of oscillatory motions in the stellar atmosphere. In: Gray, D.F., Linsky, J.L. (eds) Stellar Turbulence. Lecture Notes in Physics, vol 114. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-09737-6_8
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DOI: https://doi.org/10.1007/3-540-09737-6_8
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