Physics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm21c..07d&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #SM21C-07
Physics
2744 Magnetotail, 2748 Magnetotail Boundary Layers, 2764 Plasma Sheet, 7509 Corona
Scientific paper
The evolution of the solar corona is influenced strongly by magnetic reconnection at current sheets. I will discuss some recent research into the role and importance of magnetic reconnection and current sheets in the heating of the solar corona, which relies on the transfer, storage and dissipation of the mechanical energy present in photospheric motion, and in the acceleration of the slow solar wind above helmet streamers. In the first example, nonlinear interactions couple coronal magnetic fields to the photospheric velocity field leading to the formation of current sheets. The resulting magnetic reconnection determines both the rate of heating and the resulting coronal topology. In the second example, linear resistive instabilities can develop in current sheets found near the cusp of helmet streamers. Reconnection produces massive plasmoids which accelerate to the speed of the slow solar wind.
No associations
LandOfFree
Magnetic Reconnection in Coronal Processes 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 Magnetic Reconnection in Coronal Processes, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic Reconnection in Coronal Processes will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-762016