Numerical simulation of twisted solar corona

dc.contributor.author	Parhi, S.
dc.contributor.author	Pandey, B. P.
dc.contributor.author	Goossens, M.
dc.contributor.author	Lakhina, G. S.
dc.date.accessioned	2024-04-16T03:50:32Z
dc.date.available	2024-04-16T03:50:32Z
dc.date.issued	1998
dc.identifier.citation	New eyes to see inside the sun and stars: pushing the limits of Helio-and Asteroseismology with new observations from the ground and from space, 185th Symposium of the International-Astronomical-Union on New Eyes to See Inside the Sun and Stars, Aug 18-22, 1997, Kyoto, Japan, Int Astron Union	en_US
dc.identifier.uri	http://library.iigm.res.in:8080/xmlui/handle/123456789/1826
dc.description.abstract	The solar corona supports a variety of waves generated by convective upwelling motion in the photosphere. In order to explain the observed coronal temperature profile, resonant absorption of MHD waves by coronal plasma (Goossens et ai, 1995) has been proposed as a possible candidate. The physical picture is that the footpoint motion in the photosphere constantly stirs the coronal plasma leading to the MHD wave generation which is then resonantly absorbed producing the enhanced heating of the corona. Here we consider the problem of MHD wave propagation in a twisted solar corona.	en_US
dc.language.iso	en	en_US
dc.subject	Numerical simulation	en_US
dc.subject	Solar corona	en_US
dc.title	Numerical simulation of twisted solar corona	en_US
dc.type	Book chapter	en_US