Emission line diagnostics for a coronal condensation

dc.contributor.author	Raju, P. K
dc.date.accessioned	2006-04-13T04:33:01Z
dc.date.available	2006-04-13T04:33:01Z
dc.date.issued	1989-09
dc.identifier.citation	BASI, Vol. 17, No. 3, pp. 70-82	en
dc.identifier.uri	http://hdl.handle.net/2248/957
dc.description.abstract	Theoretical line emission rates for the coronal ions Fe X, Fe XI, FE XIII, Fe XIV, Ca XII, Ca XIII, and Ca XV, have been used to obtain various line intensity ratios as a function of electron density and electron temperature. The lines are due to the forbidden transitions in the visible part of the spectrum. With the help of these theoretical line intensity ratios physical parameters for a coronal condensation observed during the eclipse of May 30, 1965 have been derived. A simple model consisting of two regions of equal path length, one at temperature of 1.25 x 10 to the 6th K and the other at 2.5 x 10 to the 6th K and with constant electron density of 5 x 10 to the 8th/cu cm, seems to explain the observed intensities. The analysis also indicates that the observed Ca XIII line intensity appears to be high by about a factor of 4	en
dc.format.extent	736226 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	Astronomical Society of Indian	en
dc.subject	Emission line disgnostics	en
dc.subject	Coronal condensations	en
dc.title	Emission line diagnostics for a coronal condensation	en
dc.type	Article	en