On ion-cyclotron-resonance heating of the corona and solar wind
- 1Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany
- 2Astrophysikalisches Institut Potsdam, Potsdam, Germany
- 3Department of Geophysics, Peking University, Beijing, China
Abstract. This paper concisely summarizes and critically reviews recent work by the authors on models of the heating of the solar corona by resonance of ions with high-frequency waves (up to the proton cyclotron frequency). The quasi-linear theory of pitch angle diffusion is presented in connection with relevant solar wind proton observations. Hybrid fluid-kinetic model equations, which include wave-particle interactions and collisions, are derived. Numerical solutions are discussed, representative of the inner corona and near-Sun solar wind. A semi-kinetic model for reduced velocity distributions is presented, yielding kinetic results for heavy ions in the solar corona. It is concluded that a self-consistent treatment of particle distributions and wave spectra is required, in order to adequately describe coronal physics and to obtain agreement with observations.