NUMERICAL TREATMENT OF HARTLE'S PERTURBATION METHOD FOR DIFFERENTIALLY ROTATING NEUTRON STARS SIMULATED BY GENERAL-RELATIVISTIC POLYTROPIC MODELS

V. S. Geroyannis () and A. G. Katelouzos ()
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V. S. Geroyannis: Astronomy Laboratory, Department of Physics, University of Patras, Greece
A. G. Katelouzos: Astronomy Laboratory, Department of Physics, University of Patras, Greece

International Journal of Modern Physics C (IJMPC), 2008, vol. 19, issue 12, 1863-1908

Abstract: 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 nonrotating 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.

Keywords: Differential rotation; methods; numerical; stars; neutron; 02.60.-x; 04.25.Dm; 04.40.Dg; 47.75.+f; 97.60.Jd (search for similar items in EconPapers)
Date: 2008
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DOI: 10.1142/S0129183108013370

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