3-D simulations of solar and stellar convection and magnetoconvection

✍ Scribed by Å. Nordlund; R.F. Stein

• Publisher: Elsevier Science
• Year: 1990
• Tongue: English
• Weight: 649 KB
• Volume: 59
• Category: Article
• ISSN: 0010-4655
• DOI: 10.1016/0010-4655(90)90161-s

✦ Synopsis

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 XiO~have been performed, and simulations with pressure ratios of 5 x 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; ( ) 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.