On resistive dissipation of Alfvén waves in an isothermal atmosphere (Q1915526)

The incompressible Alfvén waves are considered in an isothermal and semibounded stellar atmosphere located at the half-space \(z\geq 0\). The medium is assumed to be a dissipative fluid of a finite electrical resistivity in presence of a uniform magnetic field oriented vertically. By applying proper boundary conditions to the solutions of the related linearized MHD equations, a wave reflection coefficient was calculated at \(z=0\), and a wave damping length was evaluated. The obtained results are discussed in terms of an application to the solar coronal heating.