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Title:
Effect of coronal elemental abundances on the radiative loss function
Authors:
Cook, J. W.; Cheng, C.-C.; Jacobs, V. L.; Antiochos, S. K.
Affiliation:
AA(U.S. Navy, Naval Research Laboratory, Washington, DC), AB(U.S. Navy, Naval Research Laboratory, Washington, DC), AC(U.S. Navy, Naval Research Laboratory, Washington, DC), AD(U.S. Navy, Naval Research Laboratory, Washington, DC)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 15, 1989, p. 1176-1183. Research supported by DOE. (ApJ Homepage)
Publication Date:
03/1989
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
High Temperature Plasmas, Photosphere, Plasma Density, Solar Atmosphere, Solar Corona, Abundance, Emission Spectra, Line Spectra, Thermal Stability
DOI:
10.1086/167268
Bibliographic Code:
1989ApJ...338.1176C

Abstract

The solar photosphere and corona abundances tabulated by Meyer (1985) and the chromospheric abundances given by Murphy (1985) are used here to recalculate radiative loss functions for equilibrium, low-density, optically thin plasmas. Results from a representative standard photospheric abundance set and from coronal and chromospheric abundance sets showing depletions of up to a factor of four in certain elemental abundances are compared. A significant difference is found for both the coronal and chromospheric abundance sets, with the peak of the radiative loss curve shifted closer to 10 to the 6th K than to the standard 2 x 10 to the 5th K found from photospheric abundances. Consequences of these new calculations, in particular for the cool loop model of Antiochos and Noci (1986), are discussed.

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