The SI II intercombination multiplet in late-type stars

Details The SI II intercombination multiplet in late-type stars The SI II intercombination multiplet in late-type stars

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.253..474d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 253, Dec. 1, 1991, p. 474-478. Research supported by De

Astronomy and Astrophysics

Astronomy

11

Late Stars, Resonance Lines, Silicon Compounds, Stellar Atmospheres, Stellar Spectra, Ultraviolet Spectra, Electron Density (Concentration), Iue, Line Spectra

Scientific paper

New atomic data are used to calculate the relative intensities of transitions within the Si II 3s(2)3p(2)P-3s3p(2) 4P intercombination multiplet for plasma parameters appropriate to late-type stellar atmospheres. These ratios are found to be significantly different from those of Dufton and Kingston, (1991), principally due to changes in the radiative rates. A comparison with line ratios for the sun (from Skylab S082B spectra) and late-type stars (from IUE data) indicates that although the new theoretical line ratios are in better agreement with observation, significant discrepancies still exist. Possible explanations for these discrepancies are briefly discussed.

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