Turbulent Mixing in Stars: Theoretical Hurdles

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.

5 pages, 1 figure, IAU Symposium 265, 2009

References in corpus (2)

• Coronae as Consequence of Large Scale Magnetic Fields in Turbulent Accretion Disks
• A Simple Model for Solar Isorotational Contours

Cited by in corpus (9)

• Common Envelope Evolution: Where we stand and how we can move forward
• Hydrodynamics of core-collapse supernovae and their progenitors
• Extreme value statistics for two-dimensional convective penetration in a pre-Main Sequence star
• 3D Simulations of Oxygen Shell Burning with and without Magnetic Fields
• Three-dimensional GRMHD Simulations of Rapidly Rotating Stellar Core-Collapse
• Spherical-shell boundaries for two-dimensional compressible convection in a star
• Comparison of two- and three-dimensional compressible convection in a pre-main sequence star
• Differential Rotation in a 3D Simulation of Oxygen Shell Burning
• The Three-Dimensional Collapse of a Rapidly Rotating 16 $M_{\odot }$ Star