Other
Scientific paper
Oct 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ans..conf..275n&link_type=abstract
In its Accreting Neutron Stars p 275-280 (SEE N83-15179 05-88)
Other
5
Neutron Stars, Stellar Interiors, Stellar Mass Accretion, Stellar Temperature, Thermonuclear Reactions, Cooling, Heating, Helium, Hydrogen, Steady State, Stellar Models, Stellar Structure, X Rays
Scientific paper
The thermal history of the accreting neutron star interior prior to the thermonuclear flash is examined. In the models, the accretion forms a steady hydrogen burning shell near the surface from which heat flows into the core. By numerical calculations for the stiff neutron star, it is found: (1) it takes approximately 500,000 for the core to reach the steady state where the heat inflow is balanced with the neutrino loss; and (2) the steady core temperature is approximately 1.1 - 1.2 x 10 to the 8th power K and the neutron star interior is almost isothermal, in particular in the helium layer. Thus the results justify the isothermal approximation for the neutron star interior at the initiation of the helium flash, which is employed in most of the thermonuclear flash models for Type I X-ray bursts.
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