Journal
INTERNATIONAL JOURNAL OF MODERN PHYSICS C
Volume 19, Issue 12, Pages 1863-1908Publisher
WORLD SCIENTIFIC PUBL CO PTE LTD
DOI: 10.1142/S0129183108013370
Keywords
Differential rotation; methods; numerical; stars; neutron
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We compute general-relativistic polytropic models of differentially rotating neutron stars. A brief description of our numerical treatment is given as follows. First, the relativistic Oppenheimer-Volkoff equations of hydrostatic equilibrium are solved for non-rotating models obeying the well-known polytropic equation of state. Then, uniform rotation assumed for such models is treated in the framework of Hartle's perturbation method; thus, corrections to mass and radius, owing to spherical and quadrupole deformations, are calculated. Next, a perturbative approach to the stellar structure up to terms of third order in the angular velocity is carried out; angular momentum, J, moment of inertia, I, rotational kinetic energy, T, and gravitational potential energy, W, are quantities drastically corrected by the third-order approach. Finally, assuming that our polytropic models satisfy a particular differential rotation law, we compute the increase in mass and in some other significant physical characteristics owing to the differential rotation.
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