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The Generation of Internal Waves

Published online by Cambridge University Press:  12 April 2016

Josefina Montalbán
Josefina Montalbán*
Affiliation:
Observatoire de Meudon, 92195 Meudon-Cedex, France

Extract

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The generation of internal waves in the radiatively stable stellar region by the turbulent motion at the boundary of the overlaying convective zone is similar to the same case in the deep ocean or in the earth atmosphere (Townsend, 1965), and can be described in a simple way as following: When an turbulent fluid element arrives at the boundary of the convective region with a non-zero momentum, it beats and it deforms the interface between both regions. This disturbance of the equilibrium state excites a train of internal waves propagating below the convective zone in the horizontal and vertical directions for the frequencies lower than the characteristic one for the stable stratification (Brunt-Väisälä frequency).

Type
III. Input physics for stellar structure
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 278 - 280
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Press, W.H.: 1981, Astrophys. J., 245, 286.CrossRefGoogle Scholar
Schatzman, E.: 1991, in Angular Momentum Evolution of Young Stars, Catalano, S. and Stauffer, J.R. Eds., Kluwer Academic Plublisher, p. 223.CrossRefGoogle Scholar
Townsend, A.A.: 1966, J. Fluid Mech., 24, 307.CrossRefGoogle Scholar