Truncated post-Newtonian neutron star model

Abstract

As a preliminary step towards simulating binary neutron star coalescing problem, we test a post-Newtonian approach by constructing a single neutron star model. We expand the Tolman-Oppenheimer-Volkov equation of hydrostatic equilibrium by the power of $c^{-2}$, where $c$ is the speed of light, and truncate at the various order. We solve the system using the polytropic equation of state with index $\Gamma =5/3,2$ and 3, and show how this approximation converges together with mass-radius relations. Next, we solve the Hamiltonian constraint equation with these density profiles as trial functions, and examine the differences in the final metric. We conclude the second `post-Newtonian' approximation is close enough to describe general relativistic single star. The result of this report will be useful for further binary studies. (Note to readers) This paper was accepted for publication in Physical Review D. [access code dsj637]. However, since I was strongly suggested that the contents of this paper should be included as a section in our group's future paper, I gave up the publication.

5 pages, RevTeX, 3 eps figs, epsf.sty, accepted for publication in PRD (Brief Report), but will not appear

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Cited by in corpus (6)

• Post-Tolman-Oppenheimer-Volkoff formalism for relativistic stars
• Building post-Newtonian neutron stars
• Padé approximants for truncated post-Newtonian neutron star models
• Gravity with Higher Derivatives in D-Dimensions
• Stellar structure model in the post-Newtonian approximation
• Neutron stars as extreme gravity probes