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Numerical simulations of semiconvection

Published online by Cambridge University Press:  01 August 2006

Guillaume P. Bascoul
Guillaume P. Bascoul*
Affiliation:
Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Centre for Mathematical Sciences, Wilberforce Road, Cambridge, CB3 0WA, United Kingdom email: [email protected]
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Abstract

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Using a semiconvective model based on thermohaline convection, we investigate the case of an expanding core of a main-sequence massive star. The numerical simulations at high Prandtl number show a flow consistent with the assumption that a dynamically neutral layer sits between the core and the radiative envelope. More simulations at low Prandtl number are needed to infer scaling laws applicable to astrophysical regimes.

Keywords

Convectiondiffusionhydrodynamicsstellar dynamicsinstabilities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 317 - 319
Copyright
Copyright © International Astronomical Union 2007

References

Schwarzschild, M. & Härm, R. 1958, ApJ 128, 348CrossRefGoogle Scholar