Physics
Scientific paper
Apr 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..703..193e&link_type=abstract
PLASMAS IN THE LABORATORY AND IN THE UNIVERSE: New Insights and New Challenges. AIP Conference Proceedings, Volume 703, pp. 193
Physics
1
Magnetohydrodynamics And Plasmas, Particle Emission, Solar Wind
Scientific paper
The solar corona is structured by the dynamics of plasmas and magnetic fields, which, at the global scales of coronal loops, prominences and helmet streamers may be described by magnetohydrodynamics. Here we will discuss the importance and role of nonlinear interactions both 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 including the coupling of coronal magnetic fields to the velocity field and emerging flux through the photosphere determine both the rate of heating and the resulting coronal topology. In the second example, linear resistive instabilities in develop nonlinearly to accelerate plasmoids into the slow wind. Once plasmoids are generated, the melon-seed force due to the overall magnetic field radial gradients is followed using an Expanding Box Model.
Dahlburg Russell B.
Einaudi Giorgio
Rappazzo A. F.
Velli M. M.
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