Ion heating due to plasma microinstabilities in coronal holes and the generation of the fast solar wind

Details Ion heating due to plasma microinstabilities in coronal holes and the generation of the fast solar wind Ion heating due to plasma microinstabilities in coronal holes and the generation of the fast solar wind

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh12a0397m&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH12A-0397

Physics

7511 Coronal Holes, 7867 Wave/Particle Interactions, 7871 Waves And Instabilities

Scientific paper

There is growing evidence that the heating of ions in coronal holes is due to cyclotron resonant damping of ion cyclotron waves. At the same time, the origin of these waves is much less understood. Recently, we suggested [Eos Trans. AGU, 82(47), Fall Meet. Suppl., Abstract SH11A-0695, 2001] that the source of the waves in the coronal holes is a heat flux coming from the Sun. The heat flux excites shear Alfven and electrostatic ion cyclotron waves through plasma microinstability, and then the waves heat the ions. We used a new view according to which the heat flux is launched intermittently by small-scale reconnection events (nanoflares) at the coronal base. This allows the heat flux to be sporadically large enough to drive the instabilities, while at the same time to satisfy the time-averaged energy requirements of the solar wind. Here we develop this model further. We show that the unstable waves can become strongly ion-resonant. This results in ion heating in the inner corona that is efficient enough, in the quasilinear limit, to generate the fast solar wind.

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