Heating and acceleration of coronal ions interacting with plasma waves through cyclotron and Landau resonance

On the basis of quasi-linear theory, the parallel and perpendicular wave he ating and acceleration rates for gyrotropic particle velocity distribution functions are derived. These rates can be used in anisotropic multicomponen t fluid equations, in order to describe the wave-particle interactions of i ons with, for examples, kinetic Alfven and electromagnetic or electrostatic ion cyclotron, respectively, magnetosonic waves propagating along or obliq uely to the mean magnetic field. The waves of coronal origin propagating aw ay from the Sun into the interplanetary medium can resonantly heat the sola r wind ions and accelerate minor ions preferentially with respect to the pr otons. Such processes are required in order to explain and understand the m easured characteristics of ion velocity distributions in the solar wind and to interpret the recent spectroscopic evidence obtained from EUV emission line measurements made by the Solar and Heliospheric Observatory (SOHO) spa cecraft, which indicate cyclotron-resonance-related line broadenings and sh ifts.