Mhd Study of Coronal Waves: A Numerical Approach |
| |
Authors: | S Parhi BP Pandey M Goossens GS Lakhina P De Bruyne |
| |
Institution: | (1) Indian Institute of Geomagnetism, Colaba, Bombay, 400 005, India;(2) Center for Plasma Astrophysics, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3001 Leuven, Belgium |
| |
Abstract: | The solar corona, modelled by a low β, resistive plasma slab sustains MHD wave propagations due to footpoint motions in the
photosphere. The density, magnetic profile and driver are considered to be neither very smooth nor very steep. The numerical
simulation presents the evolution of MHD waves and the formation of current sheet. Steep gradients in slow wave at the slab
edges which are signature of resonance layer where dissipation takes place are observed. Singularity is removed by the inclusion
of finite resistivity. Dissipation takes place around the resonance layer where the perturbation develops large gradients.
The width of the resonance layer is calculated. The thickness of the Alfvén resonance layer is more than that of the slow
wave resonance layer. Attempt is made to distinguish between slow and Alfvén wave resonance layers. Fast waves develop into
kink modes. As plasma evolves the current sheets which provide the heating at the edges gets distorted and fragment into two
current sheets at each edge which in turn come closer when the twist is enhanced.
This revised version was published online in July 2006 with corrections to the Cover Date. |
| |
Keywords: | |
本文献已被 SpringerLink 等数据库收录! |
|