Thermonuclear runaways at the surface of slowly accreting neutron stars

Details Thermonuclear runaways at the surface of slowly accreting neutron stars Thermonuclear runaways at the surface of slowly accreting neutron stars

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ans..conf..241b&link_type=abstract

In Max-Planck Inst. Phys. and Astrophys. Accreting Neutron Stars p 241-243 (SEE N83-15179 05-88)

Astronomy and Astrophysics

Astrophysics

3

Gamma Ray Bursts, Neutron Stars, Stellar Mass Accretion, Stellar Models, Thermonuclear Reactions, Astrophysics, Companion Stars, Equilibrium Equations, Gravitational Effects, Helium, Hydrogen, Nonthermal Radiation, Stellar Magnetic Fields

Scientific paper

Thermonuclear runaways at the surface of neutron stars with mass accretion rates of the order of 10 to the -15th power solar mass/yr/sq km are discussed. This slow accretion results in longer recurrence time scales, of the order of a few years; the shell temperature between two bursts is also lower and consequently the accreted material is pushed to higher densities before the flash. A strong magnetic field causes non-thermal emission during the flash, and may explain the gamma-ray emission. Moreover, it focusses the accretion onto the polar caps. The accretion rate per unit surface may then be 1000 times larger than the rate which result from spherical accretion. The possibility of producing hydrogen-helium flashes in such conditions is investigated. In a previous paper it was found that a metallicity Z = .04 in the accreted layer, thermonuclear instabilities where obtained when the accretion rate was larger than a critical value. However depletion of the C, N, and O nuclei due to gravitational settling seriously affect these results.

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