Quantitative spectroscopy of B supergiants in the Galaxy, the LMC and the SMC. I - The B0.5 IA supergiants Kappa Orionis, SK - 68 deg 41 and SK 159

Details Quantitative spectroscopy of B supergiants in the Galaxy, the LMC and the SMC. I - The B0.5 IA supergiants Kappa Orionis, SK - 68 deg 41 and SK 159 Quantitative spectroscopy of B supergiants in the Galaxy, the LMC and the SMC. I - The B0.5 IA supergiants Kappa Orionis, SK - 68 deg 41 and SK 159

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..498l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 498-507.

Astronomy and Astrophysics

Astrophysics

54

Early Stars, Local Thermodynamic Equilibrium, Magellanic Clouds, Stellar Composition, Stellar Mass, Supergiant Stars, Abundance, Carbon, Helium, Magnesium, Nitrogen, Oxygen, Silicon

Scientific paper

Non-LTE model-atmosphere and line-formation calculations are utilized to distinguish the components of high-resolution spectra from the B supergiants. Stellar parameters are computed from the results and presented including Teff, log g, and the ratios of helium to hydrogen and of gravitational mass to solar mass. Also determined are the elemental abundances for C, N, O, Mg, and Si. The primary result of the analysis of SK 159 and Sk - 68 deg 41 is confirmation of previous findings regarding the LMC and SMC. The idea is advanced that mass loss and mixing processes combined to enhance the CNO-processed material and consequently the He content of the two supergiants, although metal abundances do not directly support this theory. Data regarding Kappa Orionis do not exclude the possibility of a normal He abundance, a fact which suggests the tenuousness of the fits for neutral He lines in the other two stars.

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