Chemical abundances from B-stars in the Magellanic Clouds

Details Chemical abundances from B-stars in the Magellanic Clouds Chemical abundances from B-stars in the Magellanic Clouds

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.156..113r&link_type=abstract

(Instituto de Astrofisica de Canarias and Comision Interministerial de Ciencia y Tecnologia, Summer School on Evolutionary Pheno

Astronomy and Astrophysics

Astrophysics

2

Abundance, B Stars, Globular Clusters, Magellanic Clouds, Stellar Composition, Balmer Series, Oxygen, Spectral Energy Distribution, Stellar Spectra

Scientific paper

Near-Main-Sequence B-stars in the Magellanic Clouds were observed with 3.6 m telescope and CASPEC at La Silla. Spectra of high resolution and high S/N-ratio were obtained. The stars are members of the blue globular clusters NGC 1818 (LMC) and NGC 330 (SMC). The spectra are used for differential abundance analyses using Iota HER as galactic reference star. Apart from CNO, the metals are underabundant by about a factor of three and four for the LMC and SMC star, respectively. The CNO pattern is interesting since, in both stars, oxygen is considerably more abundant than carbon.

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