On the theory of silicon spectra in O and B stars

Details On the theory of silicon spectra in O and B stars On the theory of silicon spectra in O and B stars

Jan 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apjs...36..143k&link_type=abstract

Astrophysical Journal Supplement Series, vol. 36, Jan. 1978, p. 143-171.

Statistics

Computation

65

B Stars, Line Spectra, O Stars, Silicon, Stellar Atmospheres, Stellar Spectra, Early Stars, Main Sequence Stars, Stellar Models, Thermodynamic Equilibrium, Ultraviolet Spectroscopy

Scientific paper

Results of a previous calculation of a grid of predicted line profiles for 36 multiplets of Si II, III, and IV over a range of model atmospheres corresponding roughly to B0-B5 in spectral type and III-IV in luminosity class are analyzed and applied to observed spectra. The overall properties of the grid of Si line equivalent widths are reviewed, the diagnostic capability of this grid is discussed, and some results are presented for the parameters of 11 B stars derived from observed Si lines. The general fit of the predictions to the observations is evaluated, and test calculations are performed to examine the effect of varying a number of important parameters. Some systematic trends in the computational results are noted which can be expressed as phenomenological 'laws'. Special attention is given to problems arising from non-LTE effects as well as to the self-consistency of analytical results obtained from unblanketed models. It is found that the Si line calculations yield good agreement in two tests for main-sequence stars between B0 and B2, but both tests give somewhat negative results for spectral types later than B2.

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