NUMERICAL METHODS FOR ASTROPHYSICAL PLASMAS.

This review covers some numerical methods used for astrophysical plasmas and centers mainly on methods developed for astrophysical problems. After general remarks on DELTA multiplied by (times) B in astrophysical MHD calculations, a first-order, one-sided finite-difference formulation is derived for spherical and cylindrical geometries, respectively, where for any given vector field A the expression DELTA multiplied by (times) ( DELTA multiplied by A) vanishes. The artificial tensor viscosity to broaden nonplanar shock fronts is briefly discussed. The major part illustrates several numerical methods used for cometary flows, solar MHD problems, pulsar magnetospheres, equilibrium and collapse of interstellar clouds and finally, supernova shock interactions with clouds. The sections on solar physics and pulsar magnetospheres are kept very short. At the end conclusions are drawn concerning astrophysical MHD calculations.