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Oscillations of Rapidly Rotating Stars

Published online by Cambridge University Press:  12 April 2016

B. Dintrans  and
M. Rieutord
B. Dintrans
Affiliation:
Observatoire Midi-Pyrénées, 14 avenue Edouard Belin, F-31400 Toulouse, France
M. Rieutord
Affiliation:
Observatoire Midi-Pyrénées, 14 avenue Edouard Belin, F-31400 Toulouse, France

Abstract

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We present numerical simulations of gravito-inertial waves propagating in radiative zones of rapidly rotating stars. A first model, using the Boussinesq approximation, allows us to study the oscillations of a quasi-incompressible stratified fluid embedded in a rapidly rotating sphere or spherical shell. In a second step, we investigate the case of a γ Doradus-type star using the anelastic approximation. Some fascinating features of rapidly rotating fluids, such as wave attractors, appear in both cases.

Type
Part 5. Theoretical Models of Classical Pulsating Stars
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 373
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Dintrans, B., Rieutord, M., & Valdettaro, L. 1999, J. Fluid Mech., 398, 271 CrossRefGoogle Scholar
Dintrans, B. & Rieutord, M. 1999, A&A, in pressGoogle Scholar
Friedlander, S. & Siegmann, W.L. 1982, J. Fluid Mech., 114, 123 Google Scholar