New determinations of element abundances in NGC 330

Details New determinations of element abundances in NGC 330 New determinations of element abundances in NGC 330

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..557s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 557-564.

Astronomy and Astrophysics

Astrophysics

35

Abundance, Globular Clusters, Magellanic Clouds, Metallicity, Supergiant Stars, Supernovae, Carbon, Europium, Hot Stars, Nitrogen, Oxygen, Stellar Models

Scientific paper

Abundances are determined for four stars of the young globular cluster NGC 330 of the Small Magellanic Cloud. If the interstellar reddening has the classical low value, the four stars turn out to have the same metallicity, which is slightly but significantly lower than the metallicity of the field stars of about the same age. If the reddening has the high value advocated by Bessell (1991), and if the temperature of the models are increased, following the decrease of the corrected color indices, the metallicity of the two cool stars is hardly changed, the metallicity of the two hot stars is increased, and becomes similar to the metallicity of the field stars, but the spectroscopic data (profile of the H-alpha line of A19, equivalent widths of the lines of different excitation potential) are not well represented by the hotter models. The pattern of the relative abundances is hardly dependent of the reddening value. It is essentially the same for the four stars. In particular, it shows essentially solar ratios for the CNO elements relative to iron. The s-process elements are not generally enhanced, but europium (r-process) is high in the four stars.

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