Realistic exact solution for the exterior field of a rotating neutron star

Pachón, Leonardo A.; Rueda, J. A.; Sanabria-Gómez, J. D.

doi:10.1103/physrevd.73.104038

Cited by 41 publications

(57 citation statements)

References 53 publications

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“…Whenever an analytic metric is used to mimic the gravitational field of a realistic neutron star [13], and then this metric is used to reproduce various observables related to neutron stars [24], it is important to use the right moments in order to build a faithful analytic metric; otherwise any physical conclusion inferred by the analytic metric would be off [23]. If quantitative conclusions are drawn while using wrong moments in the analytic metric, they should be taken into account with some reservation.…”

Section: Consequences Of Evaluating the Right Momentsmentioning

confidence: 99%

Revising the Multipole Moments of Numerical Spacetimes and its Consequences

2012

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Identifying the relativistic multipole moments of a spacetime of an astrophysical object that has been constructed numerically is of major interest, both because the multipole moments are intimately related to the internal structure of the object, and because the construction of a suitable analytic metric that mimics a numerical metric should be based on the multipole moments of the latter one, in order to yield a reliable representation. In this note we show that there has been a widespread delusion in the way the multipole moments of a numerical metric are read from the asymptotic expansion of the metric functions. We show how one should read correctly the first few multipole moments (starting from the quadrupole mass-moment), and how these corrected moments improve the efficiency of describing the metric functions with analytic metrics that have already been used in the literature, as well as other consequences of using the correct moments.

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Section: Consequences Of Evaluating the Right Momentsmentioning

confidence: 99%

Revising the Multipole Moments of Numerical Spacetimes and its Consequences

2012

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“…Kluźniak et al 1990;Shibata & Sasaki 1998;Pachón et al 2006Pachón et al , 2012Bakala et al 2012;Gutierrez et al 2013). It has been shown that for geodesic motion, these are well described by formulae derived considering NS spacetime approximated by the Hartle-Thorne metric (Hartle & Thorne 1968;Abramowicz et al 2003;Berti et al 2005).…”

Section: Behaviour Of Isco Radius and Ns Compactnessmentioning

confidence: 82%

Appearance of innermost stable circular orbits of accretion discs around rotating neutron stars

Török

Urbanec

Adámek

et al. 2014

A&A

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The innermost stable cicular orbit (ISCO) of an accretion disc that orbits a neutron star (NS) is often assumed to be a unique prediction of general relativity. However, it has been argued that ISCO also appears around highly elliptic bodies described by Newtonian theory. In this sense, the behaviour of an ISCO around a rotating oblate neutron star is formed by the interplay between relativistic and Newtonian effects. Here we briefly explore the consequences of this interplay using a straightforward analytic approach as well as numerical models that involve modern NS equations of state. We examine the ratio K between the ISCO radius and the radius of the neutron star. We find that, with growing NS spin, the ratio K first decreases, but then starts to increase. This non-monotonic behaviour of K can give rise to a neutron star spin interval in which ISCO appears for two very different ranges of NS mass. This may strongly affect the distribution of neutron stars that have an ISCO (ISCO-NS). When (all) neutron stars are distributed around a high mass M 0 , the ISCO-NS spin distribution is roughly the same as the spin distribution corresponding to all neutron stars. In contrast, if M 0 is low, the ISCO-NS distribution can only have a peak around a high value of spin. Finally, an intermediate value of M 0 can imply an ISCO-NS distribution divided into two distinct groups of slow and fast rotators. Our findings have immediate astrophysical applications. They can be used for example to distinguish between different models of high-frequency quasiperiodic oscillations observed in low-mass NS X-ray binaries.

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“…In this regard, one can think about potential importance the equatorially symmetric configurations of the extended triple-Kerr [37,38] and quadruple-Kerr [39] solutions might have for astrophysical applications in the future. …”

Section: Discussionmentioning

confidence: 99%

Exterior field of slowly and rapidly rotating neutron stars: Rehabilitating spacetime metrics involving hyperextreme objects

Manko

Ruiz

2016

Phys. Rev. D

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The 4-parameter exact solution presumably describing the exterior gravitational field of a generic neutron star is presented in a concise explicit form defined by only three potentials. In the equatorial plane, the metric functions of the solution are found to be given by particularly simple expressions that make them very suitable for the use in concrete applications. Following Pappas and Apostolatos, we perform a comparison of the multipole structure of the solution with the multipole moments of the known physically realistic Berti-Stergioulas numerical models of neutron stars to argue that the hyperextreme sectors of the solution are not less (but possibly even more) important for the correct description of rapidly rotating neutron stars than the subextreme sector involving exclusively the black-hole constituents. We have also worked out in explicit form an exact analog of the well-known Hartle-Thorne approximate metric.

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Realistic exact solution for the exterior field of a rotating neutron star

Cited by 41 publications

References 53 publications

Revising the Multipole Moments of Numerical Spacetimes and its Consequences

Revising the Multipole Moments of Numerical Spacetimes and its Consequences

Appearance of innermost stable circular orbits of accretion discs around rotating neutron stars

Exterior field of slowly and rapidly rotating neutron stars: Rehabilitating spacetime metrics involving hyperextreme objects

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