Turbulent dissipation in the solar wind and corona

Details Turbulent dissipation in the solar wind and corona Turbulent dissipation in the solar wind and corona

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..427m&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 427-4

Physics

12

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind

Scientific paper

Models based upon anisotropic magnetohydrodynamic (MHD) cascade offer promising explanations for observations of both interplanetary and coronal turbulence and heating, which are reviewed here. In the standard picture the cascade proceeds by driving at the energy-containing scales, transfers through the inertial range, and into small scales where it drives small-scale random turbulent reconnection events. In order to understand more fully the heating and dissipation processes, one also needs to understand how small-scale MHD-driven reconnection - involving current sheets and filaments - induces kinetic plasma processes that thermalize the fluid energy. Here we suggest that in these reconnection sites MHD electric fields drive ion beam instabilities and nonlinear electron dynamics involving electron solitary wave structures, in analogy with the kinetic physics observed near parallel electric field auroral regions by the FAST spacecraft.

Affiliated with

Also associated with

No associations

Rating

Turbulent dissipation in the solar wind and corona does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Turbulent dissipation in the solar wind and corona, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Turbulent dissipation in the solar wind and corona will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1149242