Güneş Kabuğunun Manyeto-Hidrodinamik Modellenmesi

Abstract

In this study, considering the Sun as an incompressible fluid, our objective was to investigate the variation of the physical changes in the 30 % outermost convective solar layer with the use equations of magneto-hydrodynamics (MHD) for both linear and non-linear cases. Maple 8 was used for studying the changes in density, pressure, temperature and magnetic field with respect to time and radius. The first order perturbation approximation was used in MHD equations while we examine the linear case. For non linear case, the Sun was accepted as a spherically symmetric star and the analytical solutions of these equations were obtained. Hydrostatics equilibrium state was taken as a Standard Solar Model (SSM) excluding both rotation and magnetic field.