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Generation of oscillatory motions in the stellar atmosphere

  • Yoji Osaki
1. The Physical Origin of Turbulence
Part of the Lecture Notes in Physics book series (LNP, volume 114)

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.

Keywords

Stellar Model Stellar Atmosphere Radial Oscillation Propagation Diagram Ionization Zone 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag 1980

Authors and Affiliations

  • Yoji Osaki
    • 1
  1. 1.Department of AstronomyUniversity of TokyoTokyoJapan

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