3D High Resolution Simulation of Stellar Convection
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**Session 41 -- Computational Astrophysics II**
*Display presentation, Wednesday, 1, 1994, 9:20-6:30*

## [41.04] 3D High Resolution Simulation of Stellar Convection

*Hao Chen, David H. Porter, Paul R. Woodward (Dept. Astron., Univ. Minnesota)*
Numerical simulations of thermally driven convection which include
both an upper convectively unstable layer and a lower stable layer
have been performed in order to study the phenomenon of convective
overshooting. 3-D simulations at a grid resolution of 128 zones
in each dimension have been performed using the PPM hydrodynamics
code. PPM treats the compressibility of the gas explicitly in this
layer over which the density varies by roughly a factor of 30.
The problem is initially set up in a 1-D static state with small
velocity perturbations. In the unstable upper layer, a slightly
super-adiabatic temperature gradient is initially applied. This
initial temperature distribution is close to that which develops
from the action of the convective instability, and therefore the
system settles into a statistically steady state relatively rapidly.
Animations of our perspective volume renderings of these 3-D
compressible, penetrative convection flows will be shown.

This work is supported by the National Science Foundation under the Grand
Challenge Application Group for Coupled Fields and Geophysical and
Astrophysical Fluid Dynamics, grant ASC-9217394.

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