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Please use this identifier to cite or link to this item: http://library.iigm.res.in:8080/xmlui/handle/123456789/1826
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dc.contributor.authorParhi, S.-
dc.contributor.authorPandey, B. P.-
dc.contributor.authorGoossens, M.-
dc.contributor.authorLakhina, G. S.-
dc.date.accessioned2024-04-16T03:50:32Z-
dc.date.available2024-04-16T03:50:32Z-
dc.date.issued1998-
dc.identifier.citationNew 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 Unionen_US
dc.identifier.urihttp://library.iigm.res.in:8080/xmlui/handle/123456789/1826-
dc.description.abstractThe 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.isoenen_US
dc.subjectNumerical simulationen_US
dc.subjectSolar coronaen_US
dc.titleNumerical simulation of twisted solar coronaen_US
dc.typeBook chapteren_US
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