Statistics – Computation
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..may.k1106l&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, May 2-5, 1996, abstract #K11.06
Statistics
Computation
Scientific paper
Magnetoconvection, or the interaction of magnetic fields with a thermally-driven plasma flow, is a phenomenon of great importance to stellar interiors---for example, it is thought to be the underlying cause of solar and stellar dynamos. Computer simulation is necessary for investigating problems of magnetoconvection because of its inherent nonlinearities. The advent of high-speed parallel computers opens up fresh possibilities for high-resolution simulation studies of the nonlinear dynamics of magnetoconvection. This presentation will outline the approach taken in parallelizing a 2D Boussinesq MHD model code designed to run on the Cornell Theory Center's IBM SP2 computer. Here, the plasma is imagined to be confined in a rotating, heated cylindrical annulus and threaded with azimuthal magnetic fields; this configuration is roughly analogous to a near-equatorial slice of the Sun. Such a geometry is germane to the study of many interesting types of nonlinear MHD waves, some of which may self-modulate or even reverse their direction of propagation (Lantz, Ph.D. thesis, 1992). Computational issues such as domain decomposition, parallel solution of a Poisson equation, and algorithmic optimization will be discussed.
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