the effect of steady flow on the physical quantities of slow magneto acoustic waves in solar coronal plasma

Damping of slow magnetohydrodynamic(mhd) waves and oscillations are believed to contribute to the heating of the solar corona. since the launch of solar space telescopes, many observational evidences for the occurrence of slow mhd waves have been detected in various structures of the solar corona. in this paper, we studied the ef- fect of steady ow of coronal plasma on the damping time and other physical quantities of slow magneto-acoustic waves in the presence of thermal conduction and compressive viscosity. the perturbed and linearized mhd equations of a owing coronal plasma are solved both analytically and numerically by mac cormack method to investigate the elect of steady ows on physical quantities of slow magneto-acoustic waves. the results of this study show that with increasing magnitude values of the mach number from 0 to 0.6 and increasing the compressive viscosity and thermal conduction coelcient with increasing the temperature from 2 to 6 mk, the oscillation periods, the damping times and the damping qualities change signicantly. also, the results of this study show that the values and limits of the physical quantities calculated for magneto-acoustic waves in a owing viscous plasma in the presence of thermal conduction at high temperatures (more than 4 mk) correspond to observational values. moreover, the results indicate that background velocity of the coronal plasma is an elective factor in the damping of slow magneto-acoustic waves. damping of slow magneto-acoustic waves in a owing solar coronal plasma is stronger than the damping of slow magneto-acoustic waves in a stationary coronal plasma. so, steady ow along with the other damping mechanisms of slow magneto-acoustic waves must be considered in theoretical models.