Slowly rotating Tolman VII solution

Abstract

We present a model of a slowly rotating Tolman VII (T-VII) fluid sphere, at second order in the angular velocity. The structure of this configuration is obtained by integrating the Hartle-Thorne equations for slowly rotating relativistic masses. We model a sequence in adiabatic and quasi-stationary contraction, by varying the tenuity parameter $R/R_{\mathrm{S}}$, where $R$ is the radius of the configuration and $R_{\mathrm{S}}$ is its Schwarzschild radius. We determined the moment of inertia $I$, mass quadrupole moment $Q$, and the ellipticity $\epsilon$, for various configurations. Similar to previous results for Maclaurin and polytropic spheroids, in slow rotation, we found a change in the behaviour of the ellipticity when the tenuity reaches a certain critical value. We compared our results of $I$ and $Q$ for the T-VII model with those predicted by the universal fittings proposed for realistic neutron stars. For the relevant range of compactness, we found that relative errors are within $10\%$, thus suggesting the T-VII solution as a very good approximation for the description of the interior of neutron stars.

22 pages, 11 figures. Revised version, analysis and discussion extended and improved, minor clarifications and references added. Matches the version accepted in CQG

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Cited by in corpus (4)

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• Horizonless star based on regular black hole with finite radius and its observational signatures
• Slowly rotating ultracompact Schwarzschild star in the gravastar limit
• Rotation-dependent $I$-Love-$Q$-$\delta M$ relations in perturbation theory