3-D simulations of solar and stellar convection and magnetoconvection

Details 3-D simulations of solar and stellar convection and magnetoconvection 3-D simulations of solar and stellar convection and magnetoconvection

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990cophc..59..119n&link_type=abstract

Computer Physics Communications, Volume 59, Issue 1, p. 119-125.

Physics

52

Scientific paper

We present the key components of a 3-D code designed for simulating the hydrodynamics and magnetohydrodynamics of stellar atmospheres and envelopes. Some particular properties of the code are: (1) the ability to handle strong stratification (extensive simulations with bottom/top pressure ratios of 3×104 have been performed, and simulations with pressure ratios of 5×106 are being initiated); (2) a detailed treatment of the radiating surface; (3) a functional form of the subgrid-scale diffusion designed to minimize the influence on resolved motions; (4) boundary conditions open to flows. The top boundary allows the transmission of short period waves, while the bottom boundary condition was designed to enforce a displacement node for radial pressure modes.

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