3D analysis of the damping of magneto-acoustic waves in coronal loops associated with flaring events

Abstract

The plasma of the solar atmosphere loses energy by radiation and need a mechanical source of heat for maintaining the temperature in equilibrium. Many studies show that magneto-acoustic waves can balance the energy in some regions of the solar atmosphere. Specifically, these waves allow us to study the gas dynamic in structures as coronal loops and also to get the values of temperature, density and magnetic field along of them. In this project, we shall analyse the contribution of the energy dissipated by magneto-acoustic waves, in coronal loops involved in M or X class flares. Through a 3D model we shall the temperature, density, sound and Alfvén velocity distributions on the loops. In the same manner, we shall determine the conditions in which the damped waves, by viscosity and thermal conduction, provide sufficient energy for maintaining the thermal equilibrium in the solar atmosphere. These studies will serve to explain the gas dynamic of Sun-like stars and other astrophysical plasmas as solar wind, protoestellar winds and winds of late-type and hot stars.