Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235..499s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 499-510.
Astronomy and Astrophysics
Astrophysics
21
Neutron Stars, Stellar Luminosity, Stellar Magnetic Fields, Stellar Temperature, Thermal Radiation, Iterative Solution, Magnetization, Precession, Surface Temperature
Scientific paper
Two-dimensional energy transport through the crust of homogeneously magnetized neutron stars is considered by iteratively solving a coupled set of nonlinear partial differential equations. Thereby self-consistent temperature and density profiles are obtained if the field strength does not exceed the value of B = 10 to the 11th G. Numerical data are interpreted and compared with the zero-field case. The results of the weak field case suggest that homogeneously magnetized neutron stars of B = 10 to the 11th G seem to cool less efficiently than their nonmagnetic counterparts. At high field strengths of B greater than 10 to the 12th G (strong field case), the physical assumptions of the cooling model are violated and the computer code provides unreliable results. In the weak field case, the two-dimensional density profiles obtained by the code reveal that a certain amount of mass is shifted from the magnetic poles toward the equatorial region of the star in order to adjust the hydrostatic equilibrium.
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