The derivation of solar coronal electron temperature from the 1(1)S-n(1)P/1(1)S-2(1)P emission-line ratios in MG XI

Details The derivation of solar coronal electron temperature from the 1(1)S-n(1)P/1(1)S-2(1)P emission-line ratios in MG XI The derivation of solar coronal electron temperature from the 1(1)S-n(1)P/1(1)S-2(1)P emission-line ratios in MG XI

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..486k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 1, 1986, p. 486-488. Research sponsored by the Aerospace Corp. a

Statistics

Computation

18

Computational Astrophysics, Electron Energy, Emission Spectra, Line Spectra, Magnesium, Solar Corona, Atomic Interactions, Solar Flares, Solar Spectra

Scientific paper

Recent R-matrix calculations of electron excitation rates for transitions in Mg XI are used to determine the theoretical emission-line ratios as a function of electron temperature. These are found to be more temperature sensitive than the normal diagnostic for He-like ions, by factors of approximately 2.6 and 5.9 respectively, between Te = 1 × 106 K and 1 × 1O7 K. Electron temperatures deduced from R1, and R2 ratios observed by the P78-1 satellite for solar flares and active regions are in excellent agreement with those previously determined by other methods.

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