Perturbative approach to the structure of rapidly rotating neutron stars
Omar BenharDipartimento di Fisica “G. Marconi,” Universitá degli Studi di Roma, “La Sapienza,” P.le A. Moro 2, 00185 Roma, ItalyValeria FerrariDipartimento di Fisica “G. Marconi,” Universitá degli Studi di Roma, “La Sapienza,” P.le A. Moro 2, 00185 Roma, ItalyLeonardo GualtieriDipartimento di Fisica “G. Marconi,” Universitá degli Studi di Roma, “La Sapienza,” P.le A. Moro 2, 00185 Roma, ItalyStefania MarassiDipartimento di Fisica “G. Marconi,” Universitá degli Studi di Roma, “La Sapienza,” P.le A. Moro 2, 00185 Roma, Italy
2005en
ABI
Annotatsiya
We construct models of rotating stars using the perturbative approach introduced by J. Hartle in 1967, and a set of equations of state proposed to model hadronic interactions in the inner core of neutron stars. We integrate the equations of stellar structure to third order in the angular velocity and show, comparing our results to those obtained with fully nonlinear codes, to what extent third order corrections are needed to accurately reproduce the moment of inertia of a star which rotates at rates comparable to that of the fastest isolated pulsars.
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