Steady-state nuclear fusion in accreting neutron-star envelopes

Details Steady-state nuclear fusion in accreting neutron-star envelopes Steady-state nuclear fusion in accreting neutron-star envelopes

Feb 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...195..735h&link_type=abstract

Astrophysical Journal, vol. 195, Feb. 1, 1975, pt. 1, p. 735-741.

Astronomy and Astrophysics

Astrophysics

88

Astronomical Models, Neutron Stars, Nuclear Astrophysics, Nuclear Fusion, Stellar Envelopes, Stellar Evolution, X Ray Sources, Binary Stars, Computerized Simulation, Helium, Hydrogen, Steady State, Thermal Instability, X Ray Stars

Scientific paper

Conditions in the envelopes of accreting neutron stars are shown to require thermonuclear burning of hydrogen and helium in thin shells. Numerical models of such envelopes are constructed for neutron stars with masses of 0.0925, 0.476, and 1.41 solar masses and for spherically symmetric accretion rates of 10 trillionths, 1 billionth, and 10 millionths of a solar mass per year. Almost all of the shells are found to be thermally unstable, with the growth rate of the instability ranging from milliseconds to months. A crude model of nonspheric accretion is also considered and found to resemble roughly the spherical accretion problem with the same accretion rate per unit area.

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