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Nuclear fusion and carbon flashes on neutron starsThis paper reports on detailed calculations of the thermal evolution of the carbon-burning shells in the envelopes of accreting neutron stars for mass-accretion rates of 1 hundred-billionth to 2 billionths of a solar mass per yr and neutron-star masses of 0.56 and 1.41 solar masses. The work of Hansen and Van Horn (1975) is extended to higher densities, and a more detailed treatment of nuclear processing in the hydrogen- and helium-burning regions is included. Results of steady-state calculations are presented, and results of time-dependent computations are examined for accretion rates of 3 ten-billionths and 1 billionth of solar mass per yr. It is found that two evolutionary sequences lead to carbon flashes and that the carbon abundance at the base of the helium shell is a strong function of accretion rate. Upper limits are placed on the accretion rates at which carbon flashes will be important.
Document ID
19780063466
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Taam, R. E. (California Univ. Berkeley, CA, United States)
Picklum, R. E. (California, University Berkeley, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
August 15, 1978
Publication Information
Publication: Astrophysical Journal
Subject Category
ASTROPHYSICS
Funding Number(s)
CONTRACT_GRANT: NGL-05-003-497
CONTRACT_GRANT: NSF AST-76-20225
Distribution Limits
Public
Copyright
Other