Late stages of the evolution of close binaries

Details Late stages of the evolution of close binaries Late stages of the evolution of close binaries

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss..99..335d&link_type=abstract

(International Astronomical Union, Colloquium on Double Stars, Physical Properties and Generic Relations, 80th, Bandung, Indones

Astronomy and Astrophysics

Astrophysics

2

Binary Stars, Stellar Evolution, Stellar Mass Accretion, Stellar Mass Ejection, X Ray Sources, Early Stars, Main Sequence Stars, Neutron Stars, Pulsars, Variable Stars, Wolf-Rayet Stars, X Ray Binaries

Scientific paper

This review discusses how close binaries can evolve through various ways of interaction into compact objects (white dwarfs, neutron stars, black holes). Low mass X-ray sources are probably descendants of low mass stars, and various channels for their production are indicated. The evolution of massive close binaries is also examined in detail and different X-ray stages are discussed. The existence of binary pulsars, e.g. PSR 1913+16, is a striking example of the fact that close binaries can loss significant fractions of their mass and angular momentum during explosive stages. Various mechanisms for the origin of the ms-pulsar PSR 1937+214 are reviewed and it is concluded that coalescence of two orbiting neutron stars is the most probable explanation for its existence.

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