Article contents
Numerical simulations of semiconvection
Published online by Cambridge University Press: 01 August 2006
Abstract
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.
- 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
- 1
- Cited by