Computer Science
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..347d&link_type=abstract
SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 347-3
Computer Science
Particle Emission, Solar Wind, Interplanetary Magnetic Fields, Solar Wind Plasma, Sources Of Solar Wind
Scientific paper
Incompressible MHD waves propagating in a non-homogeneous background, with Alfven speed parallel gradients, can interact with their reflections producing a strong turbulent energy cascade to small perpendicular length scales. In an open magnetic region, with a strong background magnetic field, this nonlinear process can be described by the reduced MHD equations, in which incompressible or weakly compressible fluctuations are transverse to the mean field and their gradients in the parallel direction are much weaker than in the perpendicular direction. The system is forced by Alfven waves injected through the bottom boundary, with characteristic perpendicular length scale, amplitude and frequency. We identify the relevant timescales of the system and propose an ordering which favors the turbulent dissipation efficiency. We have applied this mechanism for the heating of the lower corona required in models of the origin of the solar wind.
Dmitruk Pablo
Matthaeus William H.
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