MHD study of coronal waves: A numerical approach

S. Parhi*, B. P. Pandey, M. Goossens, G. S. Lakhina, P. De Bruyne

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

5 Citations (Scopus)


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.

Original languageEnglish
Pages (from-to)147-162
Number of pages16
JournalAstrophysics and Space Science
Issue number1
Publication statusPublished - 1997
Externally publishedYes


Dive into the research topics of 'MHD study of coronal waves: A numerical approach'. Together they form a unique fingerprint.

Cite this