Dissipation and wave-ion interaction in the solar wind: Links between fluid and kinetic theory

In this paper we establish links between turbulence dissipation and wave-pa rticle interactions in the solar corona and wind. Based on quasilinear theo ry, a set of anisotropic, multi-component fluid equations is derived, which describe the wave-particle interactions of ions with Alfven waves and ion- cyclotron waves or magnetosonic waves propagating along the mean magnetic f ield. The associated equations for the wave spectrum and the heating and ac celeration of the ions are derived. In fast solar wind streams heavy ions h ave about equal thermal speeds as the protons and flow faster than them. In order to explain the observed relations, T-j/T-p approximate to m(j)/m(p) and U-j-U-p approximate to V-A, a numerical fluid-type model is developed, which takes into account the relevant wave-particle interactions. It is sho wn that left- and right-handed polarized waves propagating away from the Su n parallel to the interplanetary magnetic field can resonantly heat and acc elerate minor ions preferentially with respect to the protons in close agre ement with the measured characteristics of ion velocity distributions. Fina lly, some results from a simple analytical model are discussed.