Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338.1176c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 15, 1989, p. 1176-1183. Research supported by DOE.
Astronomy and Astrophysics
Astrophysics
121
High Temperature Plasmas, Photosphere, Plasma Density, Solar Atmosphere, Solar Corona, Abundance, Emission Spectra, Line Spectra, Thermal Stability
Scientific paper
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.
Antiochos Spiro K.
Cheng Chung-Chieh
Cook William J.
Jacobs Verne L.
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