Dynamical instability in accreting white dwarfs

Details Dynamical instability in accreting white dwarfs Dynamical instability in accreting white dwarfs

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.169...25g&link_type=abstract

(IAU, European Regional Astronomy Meeting on New Windows to the Universe, 11th, La Laguna, Spain, July 3-8, 1989) Astrophysics a

Astronomy and Astrophysics

Astrophysics

1

Dynamic Stability, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, X Ray Binaries, Carbon Monoxide, Gravitational Collapse, Neutron Stars, Stellar Models

Scientific paper

The paper studies the evolution of solid, CO white dwarfs after explosive carbon ignition at central densities around 10 to the 10th g/cu cm triggered by steady accretion in a close binary system, in order to elucidate whether these stars can collapse to form a neutron star. It is shown that as long as the velocity of the burning front remains below a critical value of 0.006c(s) (60 km/s), gravitational collapse is the final fate. These calculations support the accretion-induced collapse scenario for the origin of a fraction of low-mass X-ray binaries.

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