The galactic distribution of chemical elements as derived from B-stars in open clusters. 2: NGC 6611, S 285, and S 289

Details The galactic distribution of chemical elements as derived from B-stars in open clusters. 2: NGC 6611, S 285, and S 289 The galactic distribution of chemical elements as derived from B-stars in open clusters. 2: NGC 6611, S 285, and S 289

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...291..757k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 291, no. 3, p. 757-764

Astronomy and Astrophysics

Astrophysics

74

Abundance, B Stars, Chemical Composition, Chemical Elements, Open Clusters, Spatial Distribution, Stellar Atmospheres, Metallicity, Spectrographs, Spectrum Analysis, Stellar Evolution, Stellar Temperature

Scientific paper

The chemical composition of the open cluster NGC 6611 and the Sharpless regions S 285 and S 289 have been analyzed, and stellar parameters (effective temperature, gravity, microturbulence) and chemical abundances of 4 unevolved B-stars in NGC 6611, 2 B-stars in S 285, and 1 B-star in S 289 are given. Line blanketed local thermodynamic equilibrium (LTE) model atmospheres and non-local thermodynamic equilibrium (NLTE) line formation calculations were used for the abundance determinations of C, N, O, Mg, Al, and Si; LTE line formation calculations were used for the abundance determination of Ne, S, and Fe. In agreement with results obtained from B-type stars in the solar neighborhood and the young open cluster NGC 6231 presented in earlier papers, all elements except neon show an average underabundance of 0.1-0.4 dex with respect to the solar value. Among the cluster stars abundance differences of 0.2-0.7 dex may be observed. First results for the galactic metallicity gradient show an insignificant value for most observed elements, except for neon and sulfur, which is in contrast to results of analyses of H II regions by Shaver et al. (1983).

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