A 1D thermonuclear model for X-ray transients

Details A 1D thermonuclear model for X-ray transients A 1D thermonuclear model for X-ray transients

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ans..conf..219w&link_type=abstract

In Max-Planck Inst. Phys. and Astrophys. Accreting Neutron Stars p 219-222 (SEE N83-15179 05-88)

Astronomy and Astrophysics

Astrophysics

Astrophysics, Cosmic X Rays, Neutron Stars, Stellar Models, Thermonuclear Reactions, Deflagration, Detonation Waves, Helium, Hydrogen, Metals, Photosphere, Stellar Envelopes, Stellar Mass Accretion

Scientific paper

The thermonuclear evolution of a 1.41 solar mass neutron star, with a radius of 14.3 km, accreting various mixtures of hydrogen, helium, and heavy elements at rates of 10 to the -11th to 10 to the -10th power solar mass/yr is examined, in conjunction with Woosley and Weaver, using a one-dimensional numerical model. Effects due to general relativity or magnetic fields are ignored. Two cases are discussed. In both models, the accretion rate is such that the hydrogen shell burns to helium in steady state, with the hydrogen burning stabilized by the beta limited CNO cycle. A thick helium shell is produced, which is eventually ignited under extremely degenerate conditions, producing a thermonuclear runaway.

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