A systematic study of Alfven wave heating and dissipative
instabilities of astrophysical plasmas is proposed. This study will incorporate a mechanism for the external excitation of Alfven waves, several mechanisms of dissipation, and a geometry suitable for the physical configurations envisaged, i.e. solar coronal flux loops, prominences, etc. Substantial parts of the required analytical and numerical tools to do this have been developed in the separate groups of the applicants and will be combined in a single effort.
The resulting theory will address the problem of the efficiency of the heating of the solar corona by means of Alfven waves, will provide insight in the connection between the spectra of ideal and dissipative magnetohydrodynamics, and will yield numerical programs for the solution of non-Hermitian eigenvalue problems of two dimensional systems (with dependence along the sturcture of the magnetic flux tube and across the magnetic surfaces).
Funding SchemeCSC - Cost-sharing contracts
3000 Louvain / Leuven