Nonlinear development of MHD waves in coronal loops

dc.contributor.author	Parhi, S.
dc.contributor.author	Pandey, B.P.
dc.contributor.author	Goossens, M.
dc.contributor.author	Lakhina, G.S.
dc.contributor.author	Bruyne, P.De
dc.date.accessioned	2017-08-09T05:36:04Z
dc.date.accessioned	2021-02-12T09:55:46Z
dc.date.available	2017-08-09T05:36:04Z
dc.date.available	2021-02-12T09:55:46Z
dc.date.issued	1997
dc.identifier.citation	Advances in Space Research, v.19/12, p.1891-1894, 1997, doi: 10.1016/S0273-1177(97)00095-1	en_US
dc.identifier.uri	http://localhost:8080/xmlui/handle/123456789/961
dc.description.abstract	The solar corona, modelled by a low β, resistive plasma slab sustains MHD wave propagations due to footpoint motions in the photosphere. The numerical simulation presents the evolution of MHD waves and the formation of current sheets. Steep gradients at the slab edges, which are signatures of resonance layers are observed. Singularities are removed by the inclusion of finite resistivity. The fast waves develop kink modes. As the plasma evolves the current sheets which provide heating at the edges fragment into two current sheets at each edge which in turn come closer when the twist is enhanced.	en_US
dc.language.iso	en	en_US
dc.subject	Nonlinear development	en_US
dc.subject	Coronal loops	en_US
dc.subject	MHD wave	en_US
dc.title	Nonlinear development of MHD waves in coronal loops	en_US
dc.type	Article	en_US
dc.identifier.accession	091281