Abstract
AbstractUsing 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.
Publisher
Cambridge University Press (CUP)
Subject
Astronomy and Astrophysics,Space and Planetary Science
Cited by
1 articles.
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