Fe I - MG II K line fluorescence in K giant and bright giant stars

Details Fe I - MG II K line fluorescence in K giant and bright giant stars Fe I - MG II K line fluorescence in K giant and bright giant stars

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.243..381h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 243, April 1, 1990, p. 381-389. Research supported by S

Astronomy and Astrophysics

Astronomy

12

Fluorescence, Giant Stars, Iron, K Stars, Magnesium, Stellar Spectra, Chromosphere, Emission Spectra, Radiative Transfer, Resonance Lines, Stellar Envelopes, Stellar Luminosity

Scientific paper

Emission lines of Fe I from the multiplet uv44 are observed at 2823.28A and 2843.98A in late-type giant and bright giant stars. It has been recognized for some time that these lines can be excited by Mg II k line radiation in the transition at 2795.54A. The first radiative transfer calculations to account for the strength of the Fe I lines Iota Aur (K3 II), Alpha Boo (K2 III), Beta Gem (K0 III) and Alpha Tau (K5 III) show that the observed Fe I is created in the chromospheres of the K stars and not in circumstellar shells, as suggested by some authors. The Fe I lines provide an additional test of model chromospheres at temperatures between those where the Mg II and Ca II resonance lines are formed.

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