Turbulent Mixing in Stars: Theoretical Hurdles

TL;DR

This paper discusses the development of 3D time-dependent simulations to study turbulence in stars, highlighting theoretical challenges and potential extensions to include rotation and magnetic effects.

Contribution

It introduces a new approach using 3D simulations for stellar turbulence and critiques the diffusive approximation in turbulent convection.

Findings

Identified limitations of diffusive models for turbulent convection

Outlined a framework for 3D hydrodynamic simulations in stellar physics

Suggested extensions to include rotation and magnetic fields

Abstract

A program is outlined, and first results described, in which fully three-dimensional, time dependent simulations of hydrodynamic turbulence are used as a basis for theoretical investigation of the physics of turbulence in stars. The inadequacy of the treatment of turbulent convection as a diffusive process is discussed. A generalization to rotation and magnetohydrodynamics is indicated, as are connection to simulations of 3D stellar atmospheres.