Solar coronal heating by magnetosonic waves

Solar coronal heating by magnetohydrodynamic (MHD) waves is investigated. u ltraviolet (UV) and X-ray emission lines of the corona show non-thermal bro adenings. The wave rms velocities inferred from these observations are of t he order of 25-60 km s(-1). Assuming that these values are not negligible, we solved MHD equations in a quasi-linear approximation, by retaining the l owest order non-linear term in rms velocity. Plasma density distribution in the solar corona is assumed to be inhomogeneous. This plasma is also assum ed to be permeated by dipole-like magnetic loops. Wave propagation is consi dered along the magnetic field lines. As dissipative processes, only the vi scosity and parallel (to the local magnetic field lines) heat conduction ar e assumed to be important. Two wave modes emerged from the solution of the dispersion relation. The fast mode magneto-acoustic wave, if originated fro m the coronal base can propagate upwards into the corona. and dissipate its mechanical energy as heat. The damping length-scale of the fast mode is of the order of 500 km. The wave energy flux associated with these waves tame d out to be of the order of 2.5 x 105 ergs cm(-2) s(-1) which is high enoug h to replace the energy lost by thermal conduction to the transition region and by optically thin coronal emission. The fast magneto-acoustic waves pr ove to be a likely candidate to heat the solar corona. The slow mode is abs ent, in other words cannot propagate in the solar corona.