An Interpretation of the Millisecond time variation in Hard X-ray solar flares

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2964

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DC Field	Value	Language
dc.contributor.author	Krishan, V	-
dc.contributor.author	Kundu, M. R	-
dc.date.accessioned	2008-07-31T05:16:29Z	-
dc.date.available	2008-07-31T05:16:29Z	-
dc.date.issued	1985	-
dc.identifier.citation	Unstable current systems and plasma instabilities in astrophysics; Proceedings of the 107th Symposium, College Park, MD, August 8-11, 1983 Dordrecht, D. Reidel Publishing Co., pp. 299-301.	en
dc.identifier.issn	A85-48801 24-90	-
dc.identifier.uri	http://hdl.handle.net/2248/2964	-
dc.description.abstract	Recent observations of the fast time variability in the hard X-ray emission from solar flares are interpreted. The fast spikes are assumed to be superimposed on the thermal X-ray emission. The rise and fall of a spike are caused by disruptions in the plasma. The rise time represents the impulsive heating time and the decay or fall time represents a quick cooling of the plasma due to the accelerating growth rate of the m = 1 tearing mode. The estimated characteristic time durations of the spike are found to be in good agreement with the observed ones.	en
dc.format.extent	244392 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	en
dc.publisher	International Astronomical Union	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1985IAUS..107..299K	en
dc.subject	X-ray emission	en
dc.subject	Solar flares	en
dc.title	An Interpretation of the Millisecond time variation in Hard X-ray solar flares	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

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