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Thermonuclear runaways on neutron starsThermonuclear runaways which develop when neutron stars of 0.476 solar masses accrete hydrogen-rich material at 10 to the -10th and 2 x 10 to the -9th solar masses/year have been followed using a numerical model. It is found that a thermal instability occurs at densities in excess of 10 to the 5th g/cu cm and that the maximum accumulated mass required to initiate the runaway is 0.7 x 10 to the -12th and 2.1 x 10 to the -12th solar masses for the mass accretion rates of 10 to the -10th and 2 x 10 to the -9th solar masses/year, respectively. Heating the of the neutron star envelope by hydrogen burning leads to the ignition of helium. The nonequilibrium burning of helium by a combination of (alpha, p), (p, gamma), and (alpha, gamma) reactions involving O-14, O-15, and other heavy nuclei provides the energy for an X-ray burst. The gross properties of these models bear suggestive resemblance to those observed for some X-ray burst sources.
Document ID
19800026541
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Taam, R. E.
(Northwestern University Evanston, Ill., United States)
Picklum, R. E.
(California, University Berkeley, Calif., United States)
Date Acquired
August 10, 2013
Publication Date
October 1, 1979
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
80A10711
Distribution Limits
Public
Copyright
Other

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