Stellar Turbulent Convection: A Self‐consistent Model

Stellar Turbulent Convection: A Selfconsistent Model

We present a selfconsistent model for stellar turbulent convection which is similar in spirit to the CM model (Canuto & Mazzitelli 1991) since it accounts for the full spectrum of the turbulent eddies rather than only one eddy, as done in the mixing length theory (MLT). The model differs from the CM model in the treatment of the rate of energy input ns(k) from the source that generates the turb...

Excitation of stellar p - modes by turbulent convection

Acoustic power and oscillation amplitudes of radial oscillations computed for a solar model are compared with solar seismic observations. The oscillations are assumed stochastically excited by turbulence. The numerical computations are based upon a theoretical formulation of the power going into solar like oscillation modes as proposed by Samadi et al. (2000) in a companion paper. This formulat...

Efficient Turbulent Compressible Convection in the Deep Stellar Atmosphere

This paper reports an application of gas-kinetic BGK scheme to the computation of turbulent compressible convection in the stellar interior. After incorporating the Subgrid Scale (SGS) turbulence model into the BGK scheme, we tested the effects of numerical parameters on the quantitative relationships among the thermodynamic variables, their fluctuations and correlations in a very deep, initial...

Turbulent Convection in Stellar Interiors. I. Hydrodynamic Simulation

We describe the results of three-dimensional (3D) numerical simulations designed to study turbulent convection in the stellar interiors, and compare them to stellar mixing-length theory (MLT). Simulations in 2D are significantly different from 3D, both in terms of flow morphology and velocity amplitude. Convective mixing regions are better predicted using a dynamic boundary condition based on t...

A Discrete Dynamical System Subgrid-Scale Model of Turbulent Convection