Chemical-abundance anomalies in AM stars and their relation to anomalies in AP stars

Details Chemical-abundance anomalies in AM stars and their relation to anomalies in AP stars Chemical-abundance anomalies in AM stars and their relation to anomalies in AP stars

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975pazh....1...26k&link_type=abstract

Pis'ma v Astronomicheskii Zhurnal, vol. 1, Dec. 1975, p. 26-31. In Russian.

Other

A Stars, Abundance, Main Sequence Stars, Metallic Stars, Stellar Atmospheres, Chemical Composition, Rare Earth Elements, Statistical Correlation, Transition Metals

Scientific paper

Abundance anomalies in 23 Am stars are analyzed, and the results are compared with data on 26 Ap stars, for the following groups of elements: (1) the light elements from C to Ca; (2) the iron group from Ti to Ni; (3) the group consisting of Sr, Y, and Zr; and (4) the rare earths. For both types of stars, it is found that the overabundances of light elements are not intercorrelated and are poorly correlated with overabundances of elements in the other groups. Good correlations are observed among the overabundances of the iron-group elements as well as between these overabundances and those of elements in groups 3 and 4. The correlations are found to be somewhat poorer for the group-3 elements, but very good for the rare earths. The correlations between the Am and Ap types are found to be identical for the rare-earth and iron-group elements, and no anticorrelations are observed. The results are shown to indicate a continuous transition from normal stars through Am stars to Ap stars. Possible mechanisms for the abundance anomalies are briefly considered.

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