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 MHD- waves 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 kg 9 1.010 .