On the mechanisms of MHD wave damping in the partially ionized solar plasmas

In order to conclude about the role of collisional friction, viscous and thermal conductivity mechanisms of MHD wave damping in the solar partially ionized plasmas, a quantitative comparative study of efficiency of all these mechanisms in different parts of the solar atmosphere is performed. All the important solar MHD modes are considered: Alfvén wave, fast magnetoacoustic wave and slow magnetoacoustic/acoustic wave. In general, the correct description of MHD wave damping requires the consideration of all energy dissipation mechanisms via the inclusion of the appropriate terms in the generalized Ohm’s law, the momentum, energy and induction equations. Specific forms of the generalized Ohm’s law and induction equation, suitable for partially ionized regions of the solar atmosphere, are presented and discussed.