Neutron star formation in low-mass binary systems

Details Neutron star formation in low-mass binary systems Neutron star formation in low-mass binary systems

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296..489l&link_type=abstract

In ESA, The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 1: X Ray Binaries p 489-491 (SEE N90-25711 19-89)

Astronomy and Astrophysics

Astronomy

Neutron Stars, Star Formation, Stellar Mass Accretion, X Ray Binaries, Star Formation Rate, Stellar Evolution, Stellar Models, White Dwarf Stars

Scientific paper

The formation of low mass X-ray binaries containing a neutron star as the compact X-ray source is discussed. The problem presented by the standard mechanism and concerning the disruption of the binary system is investigated. Two solutions are possible: either the neutron star forms isolately, and only later binds with a relatively low-mass star, or it forms in situ. It is shown that the accretion induced collapse of CO white dwarfs is possible for a limiting range of initial conditions. In contrast, ONeMg white dwarfs appears less likely.

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