Spatial profiles of lines in active region loops

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3801

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DC Field	Value	Language
dc.contributor.author	Krishan, V	-
dc.date.accessioned	2008-09-23T09:48:35Z	-
dc.date.available	2008-09-23T09:48:35Z	-
dc.date.issued	1983-10	-
dc.identifier.citation	Solar Physics, Vol. 88, No. 1 - 2, pp. 155 - 161	en
dc.identifier.issn	0038-0938	-
dc.identifier.uri	http://hdl.handle.net/2248/3801	-
dc.description.abstract	From the statistical treatment of magnetohydrodynamically turbulent plasma, a steady-state density, temperature and magnetic field structure is derived for a coronal loop emitting in UV and EUV range. Spatial variation of line flux is presented for the lines C II, C III, O IV, O VI, Ne VII, and Mg X. It is found that the hotter lines which are emitted near the surface of the loop have larger spatial extents compared to the lines originating in the cool core of the loop, in agreement with the observations.	en
dc.language.iso	en	en
dc.publisher	Springer	en
dc.relation.uri	http://www.springerlink.com/content/r9n6147g28w22304/	en
dc.subject	Coronal Loops	en
dc.subject	Line Shape	en
dc.subject	Solar Activity Effects	en
dc.subject	Solar Corona	en
dc.subject	Solar Spectra	en
dc.subject	Ultraviolet Spectra	en
dc.subject	Astronomical Models	en
dc.subject	Magnetic Field Configurations	en
dc.subject	Magnetohydrodynamic Turbulence	en
dc.subject	Plasma Turbulence	en
dc.subject	Solar Physics	en
dc.subject	Temperature Distribution	en
dc.title	Spatial profiles of lines in active region loops	en
dc.type	Article	en
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