Structure of the Solar Corona

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/188

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DC Field	Value	Language
dc.contributor.author	Krishan, V	-
dc.date.accessioned	2005-01-08T05:29:09Z	-
dc.date.available	2005-01-08T05:29:09Z	-
dc.date.issued	1988	-
dc.identifier.citation	Kodaikanal Observatory Bulletins Series A, Vol. 9, pp. 81-88	en
dc.identifier.issn	0374-3632	-
dc.identifier.uri	http://hdl.handle.net/2248/188	-
dc.description.abstract	Solar eclipses established the existence of the outer region of the solar atmosphere, the solar corona, extending to several solar-radii and exhibiting open and closed magnetic field patterns. The density and the temperature of the solar corona were inferred from the optical spectrum. Through the use of coronagraphs on and above the earth and finally on the skylab and with enlarged range of spectral, spatial and temporal resolutions, a multitude of structures formed by the complex intraplay of density, temperature and magnetic field gradients, have been revealed. The morphology and dynamics of these structures which set up a link between the interior of the sun and the solar wind, are briefly described in this review.	en
dc.format.extent	1194729 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	-
dc.publisher	Indian Institute of Astrophysics, Bangalore	en
dc.subject	Solar Corona	en
dc.subject	Solar Eclipse	en
dc.subject	Coronography	en
dc.title	Structure of the Solar Corona	en
dc.type	Article	en
Appears in Collections:	IIAP Publications Kodaikanal Observatory Bulletins (1905 - 1997 )

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