Modelling of Solar Coronal Oscillations

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/248

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DC Field	Value	Language
dc.contributor.author	Krishan, V	-
dc.date.accessioned	2005-01-18T04:13:30Z	-
dc.date.available	2005-01-18T04:13:30Z	-
dc.date.issued	1997	-
dc.identifier.citation	Kodaikanal Observatory Bulletins Series A, Vol. 13, pp. 87-90	en
dc.identifier.issn	0374-3632	-
dc.identifier.uri	http://hdl.handle.net/2248/248	-
dc.description.abstract	The study of coronal osciallations is important since these oscillations could be responsible for the heating of the solar corona. Coronal structures are ex[ected to undergo three types of oscillations - non-compressional Alfven waves and the compressional slow and fast magnetosonic waves. Since the data from the eclipse of October 24, 1995 shows intensity oscillaitons, these are interpreted as the slow and or fast magnetosonic modes. The corresponding values of the plasma parameters as well as an estimate of the flux in these modes is also given.	en
dc.format.extent	75538 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	-
dc.publisher	Indian Institute of Astrophysics, Bangalore	en
dc.subject	Coronal oscillations	en
dc.subject	Slow and fast magnetosonic waves	en
dc.subject	Coronal heating	en
dc.title	Modelling of Solar Coronal Oscillations	en
dc.type	Article	en
Appears in Collections:	IIAP Publications Kodaikanal Observatory Bulletins (1905 - 1997 )

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