Statistics – Computation
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apjs...75..449v&link_type=abstract
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 75, Feb. 1991, p. 449-462. DOE-supported research.
Statistics
Computation
98
Neutron Stars, Stellar Evolution, Stellar Interiors, Stellar Temperature, X Ray Stars, Computational Astrophysics, Stellar Mass, Stellar Models
Scientific paper
A model is presented for calculating the evolution of neutron stars in the thermal evolution approximation, which follows the detailed temperature dependence in the interior of the star assuming a fixed density structure. A new numerical algorithm for solving the thermal evolution equations is presented and comparisons are made with other algorithms. The neutrino emissivities, heat capacities, thermal conductivities, and superfluid treatment used in the models are described. Results of the thermal evolution model are presented for representative neutron star models of a gravitational mass M = 1.4 solar mass with and without strong surface magnetic fields, and also for stars with a central accelerated cooling mechanism. Isothermal cooling models are examined to determine the ages beyond which the cooling model applies.
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