Magnetohydrodynamic Computer Simulation of Erupting Low Solar Coronal Magnetic Fields

Abstract

An analytical solution of initial and un-sheared low solar coronal magnetic arcade as initial value is perturbed and equilibrium is assumed to loss. The dynamical state of lossing equilibrium is descibed first and possible consequnces to the numerical scheme is derived. The dynamical evolution is followed by computer simulation which computed numerical solutions of complete set time-dependent magnetohydrodynamics partial differential equations. Automatic algorithm to inspect the MHD fast-mode speed is introduced to maintain simulation scheme stable during computations. Results show there will be shocks, known as MHDwaves

shock, along the way to interplanetary space. Temperature shock is not prominent and only a relatively unsignificant temperature rise is resulted, instead density shock is noticeable. The density rise is relatively far greater to order of 100.1  9 kg .