The binary system Sirius in the context of stellar evolution

Details The binary system Sirius in the context of stellar evolution The binary system Sirius in the context of stellar evolution

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...114..289d&link_type=abstract

Astronomy and Astrophysics, vol. 114, no. 2, Oct. 1982, p. 289-296.

Astronomy and Astrophysics

Astronomy

4

Binary Stars, Stellar Evolution, Stellar Mass Ejection, White Dwarf Stars, Stellar Atmospheres, Stellar Coronas, Stellar Models, X Ray Astronomy

Scientific paper

In light of simple assumptions concerning the dynamical evolution of the system Sirius, the evolution of Sirius B from an initial mass of 3.75-5.2 solar masses has not been influenced by the presence of a companion, but rather proceeded like that of a single star, through stellar wind mass loss and planetary nebula ejection. Following the Iben and Truran (1978) modelling of the s-process nucleosynthesis in the envelopes of thermally pulsing stars, the composition of the planetary nebula ejected by initial progenitors of masses allowed by the dynamical evolution can be derived. The anticorrelation of CNO abundances and s-process elements in Sirius A is at variance with the results obtained in this framework, while it is in agreement with diffusion theory predictions.

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