On the evolution of slowly accreting neutron stars

Details On the evolution of slowly accreting neutron stars On the evolution of slowly accreting neutron stars

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...399..634b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 2, p. 634-645.

Astronomy and Astrophysics

Astrophysics

14

Gamma Ray Bursts, Neutron Stars, Stellar Evolution, Stellar Mass Accretion, Abundance, Accretion Disks, Nuclear Fusion

Scientific paper

In the light of recent calculations of pycnonuclear reaction rates for light elements, we consider the problem of slow interstellar accretion onto old, possibly magnetized neutron stars. We argue that accretion will occur at the Hoyle-Lyttleton rate after the star has spun down in less than about 10 exp 9 yr. A deep ocean of liquid hydrogen and helium, extending down to depths about 100 m, will cover the surface of the star once it has accreted about 10 exp 25 g of gas. Beneath the ocean will be a layer of almost pure solid O-16 which undergoes two-stage electron capture to C-16 above a pressure 2.7 x 10 exp 28 dyne/sq cm, corresponding to an accreted mass of about 10 exp 27 g. Taking into account the presence of multiple layers of distinct chemical composition, we conclude that the crust will be stable to small perturbations under the conditions envisaged for instellar accretion. A thick layer of up to 10 exp 27 g of metastable C-16 will then accumulate. We discuss the implications of these results to old Galactic neutron stars as sources of gamma-ray bursts.

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