Abstract
The Barium stars are reviewed in terms of their known binary nature and their quantitative abundance peculiarities. It is concluded that the most likely explanation of the 12C and s-process overabundances observed in the Barium stars is mass transfer from a companion, which is now a white dwarf, but was once a 4He-burning thermally-pulsing asymptotic giant branch star.
Publisher
Cambridge University Press (CUP)