Coronal magnetic field measurements using forbidden emission lines

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DC Field	Value	Language
dc.contributor.author	Megha, A	-
dc.contributor.author	Sampoorna, M	-
dc.contributor.author	Nagendra, K. N	-
dc.contributor.author	Sankarasubramanian, K	-
dc.date.accessioned	2020-11-11T07:44:16Z	-
dc.date.available	2020-11-11T07:44:16Z	-
dc.date.issued	2018-02	-
dc.identifier.citation	Proceedings of the International Astronomical Union, Vol. 340, pp. 61-62	en_US
dc.identifier.issn	1743-9213	-
dc.identifier.uri	http://prints.iiap.res.in/handle/2248/6914	-
dc.description	Restricted Access © International Astronomical Union https://doi.org/10.1017/S1743921318001023	en_US
dc.description.abstract	The polarization measurement of coronal forbidden emission lines is the most promising method of determining the direction of magnetic fields in the corona. A classical theory for the forbidden lines was presented in Megha et al. (2017) for the case of arbitrary strength magnetic fields. Here we apply that theoretical formalism to study the effect of density distributions, magnetic field configurations, and velocity fields on the Stokes profiles formed in corona. For illustrations we use the atomic parameters of the [Fe xiii] 10747 ˚A coronal forbidden line.	en_US
dc.language.iso	en	en_US
dc.publisher	Cambridge University Press	en_US
dc.subject	Sun: corona	en_US
dc.subject	Sun: magnetic fields	en_US
dc.subject	Line: profiles - polarization	en_US
dc.title	Coronal magnetic field measurements using forbidden emission lines	en_US
dc.type	Article	en_US
Appears in Collections:	IIAP Publications

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