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Evolution of the sun with mixing by hydrodynamic instabilities

Published online by Cambridge University Press:  04 August 2017

Wai-Yuen Law ,
E. Knobloch  and
H.C. Spruit
Wai-Yuen Law
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, 8046 Garching bei München, FRG
E. Knobloch
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, 8046 Garching bei München, FRG
H.C. Spruit
Affiliation:
Max-Planck-Institut für Physik und Astrophysik, 8046 Garching bei München, FRG

Extract

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Following Schatzman and Maeder (1981) we compute the evolution of the sun with partial mixing by hydrodynamic instabilities. Instead of simply assuming a turbulent diffusion coefficient which is a constant multiple of the viscosity, we incorporate some of the properties of hydrodynamic instabilities. This puts limits on the amount of diffusion that can be obtained, and makes it dependent on time and position in the star.

Type
III. BINARITY, PULSATION, ROTATION AND MIXING
Information
Symposium - International Astronomical Union , Volume 105: Observational Tests of the Stellar Evolution Theory , 1984 , pp. 523 - 524
Copyright
Copyright © Reidel 1984 

References

Berthomieu, G., Provost, J., Schatzman, E., preprint.Google Scholar
Knobloch, E., Spruit, H.C.:1983, Astron. Astrophys. 125, p. 59.Google Scholar
Schatzman, E., Maeder, A.: 1981, Astron. Astrophys. 96, p. 1.Google Scholar
Skumanich, A.: 1972, Astrophys. J. 171, p. 565.CrossRefGoogle Scholar