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Core saturation in a moving mediumA numerical technique for solving the line transfer equation of a two-level atom in static equilibrium is presented. Complete redistribution of emitted photons is assumed, as is saturation at the line core. Emission intensity is calculated either by a generalized Eddington-Barber relation, a first-order differential equation for the specific intensity, or by a formal transfer integral. Sample calculations are performed of the line transfer equation in a semi-infinite atmosphere with a constant Planck function of the collision parameter and for the Mg II resonance line in a model solar atmosphere experiencing shocks. Attention is focused on the line wings in the latter problem. The first order differential equation approach yields the best intensity values and temperature structure.
Document ID
19850033979
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Kalkofen, W.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Ulmschneider, P.
(Heidelberg, Universitaet Heidelberg, Germany)
Date Acquired
August 12, 2013
Publication Date
January 1, 1984
Subject Category
Astrophysics
Accession Number
85A16130
Funding Number(s)
CONTRACT_GRANT: DFG-SFB-132
CONTRACT_GRANT: NAGW-253
Distribution Limits
Public
Copyright
Other

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