Statistics – Computation
Scientific paper
Jan 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...227...61s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 227, no. 1, Jan. 1990, p. 61-70.
Statistics
Computation
29
Computational Astrophysics, Magnetic Stars, Neutron Stars, Stellar Cores, Stellar Temperature, Astronomical Models, Density Distribution, Equations Of State, Stellar Magnetic Fields, Stellar Rotation, Thermal Radiation
Scientific paper
Temperature and density profiles of homogeneously magnetized neutron stars were calculated by solving a coupled set of nonlinear-structure equations longitudinal and transverse to a quantizing magnetic field supposed to exist in the crust of a neutron star. It is shown that the equatorial surface temperature of a strongly magnetized neutron star is significantly decreased compared to the zero-field case, while the polar temperature is slightly increased. Interpreting these results with respect to the cooling efficiency of homogeneously magnetized neutron stars, it is concluded that the two opposite effects either cancel each other or reduce the cooling rates compared to equivalent nonmagnetic stars.
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