Physics
Scientific paper
Jun 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.508..395m&link_type=abstract
In: Proceedings of the SOHO 11 Symposium on From Solar Min to Max: Half a Solar Cycle with SOHO, 11-15 March 2002, Davos, Switze
Physics
Solar Coronal Holes, Solar Wind
Scientific paper
A scenario is suggested for coronal heating in which reconnection in the chromospheric network is assumed to create high-frequency waves. They are considered as the main energy source for the heating of the solar corona and generation of the fast solar wind. Multi-fluid models have been developed, which include on the basis of quasilinear theory (QLT) the damping of the waves. It is shown that a self-consistent treatment of wave damping and absorption is necessary. QLT predicts that ions in resonance with ion-cyclotron waves suffer merely pitch-angle diffusion. Evidence for this process is found in Helios solar wind data. In the numerical results obtained from a semi-kinetic model for a coronal hole, the ion velocity distributions show also a "plateau", which is defined by a vanishing pitch-angle gradient at the resonance and implies marginal stability.
Marsh E.
Tu Chia-Ying
Vocks Christian
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