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Effect of coronal elemental abundances on the radiative loss function
Cook, J. W.; Cheng, C.-C.; Jacobs, V. L.; Antiochos, S. K.
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)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 15, 1989, p. 1176-1183. Research supported by DOE. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
High Temperature Plasmas, Photosphere, Plasma Density, Solar Atmosphere, Solar Corona, Abundance, Emission Spectra, Line Spectra, Thermal Stability
Bibliographic Code:


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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