Various features of quasiequilibrium sequences of binary neutron stars in general relativity

Taniguchi, Keisuke; Gourgoulhon, Éric

doi:10.1103/physrevd.68.124025

Cited by 63 publications

(104 citation statements)

References 71 publications

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“…The French [23,24,49,50] and Japanese [26,27] numerical groups also make these assumptions but do not see compression. Further, Wilson [51] examined the head-on collision of two NSs using both the SCF/quasi-equilibrium conditions and in full general relativity.…”

Section: A Compression In Irrotational Simulationsmentioning

confidence: 99%

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Favata

2006

Phys. Rev. D

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Numerical simulations of binary neutron stars by Wilson, Mathews, and Marronetti indicated that neutron stars that are stable in isolation can be made to collapse to black holes when placed in a binary. This claim was surprising as it ran counter to the Newtonian expectation that a neutron star in a binary should be more stable, not less. After correcting an error found by Flanagan, Wilson and Mathews found that the compression of the neutron stars was significantly reduced but not eliminated. This has motivated us to ask the following general question: Under what circumstances can general relativistic tidal interactions cause an otherwise stable neutron star to be compressed? We have found that if a non-rotating neutron star possesses a current quadrupole moment, interactions with a gravitomagnetic tidal field can lead to a compressive force on the star. If this current quadrupole is induced by the gravitomagnetic tidal field, it is related to the tidal field by an equation-of-state-dependent constant called the gravitomagnetic Love number. This is analogous to the Newtonian Love number that relates the strength of a Newtonian tidal field to the induced mass quadrupole moment of a star. The compressive force is almost never larger than the Newtonian tidal interaction that stabilizes the neutron star against collapse. In the case in which a current quadrupole is already present in the star (perhaps as an artifact of a numerical simulation), the compressive force can exceed the stabilizing one, leading to a net increase in the central density of the star. This increase is small ( 1%) but could, in principle, cause gravitational collapse in a star that is close to its maximum mass. This paper also reviews the history of the Wilson-MathewsMarronetti controversy and, in an appendix, extends the discussion of tidally-induced changes in the central density to rotating stars.

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Section: A Compression In Irrotational Simulationsmentioning

confidence: 99%

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Favata

2006

Phys. Rev. D

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“…Finally in Ref. [16] calculations were presented for an extensive sample of values of Γ and of M/R, for both equal and unequal masses. Comparison of the endpoints of their sequences of models with those of Uryu et al [30,31,32] showed good agreement [16].…”

Section: Quasiequilibrium Binary Neutron Star Initial Configuratmentioning

confidence: 99%

“…(2.5a). Also plotted as dashed curves with data points are the corresponding "virial" errors V E(M ), computed from the numerical data, and tabulated in [15,16], where…”

Section: Quasiequilibrium Binary Neutron Star Initial Configuratmentioning

confidence: 99%

“…Alternatively, for example, one can leave the eccentricity as a free parameter and solve for that value that gives the best agreement between the PN and the numerical results for the given angular velocity. In comparing with the non-spinning NS-NS initial data sets of [14,15,16], our main results can be summarized using Fig. 1.…”

Section: Introductionmentioning

confidence: 99%

“…In Sec. III we consider the catalogue of quasiequilibrium NS-NS sequences computed by the Meudon group [14,15,16]. Section IV considers NS-BH binaries obtained by Taniguchi et al [17,18,19] and Grandclément [20].…”

Section: Introductionmentioning

confidence: 99%

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Post-Newtonian diagnosis of quasiequilibrium configurations of neutron star–neutron star and neutron star–black hole binaries

Berti¹,

Iyer²,

Will³

2008

Phys. Rev. D

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We use a post-Newtonian diagnostic tool to examine numerically generated quasiequilibrium initial data sets for non-spinning double neutron star and neutron star-black hole binary systems. The PN equations include the effects of tidal interactions, parametrized by the compactness of the neutron stars and by suitable values of "apsidal" constants, which measure the degree of distortion of stars subjected to tidal forces. We find that the post-Newtonian diagnostic agrees well with the double neutron star initial data, typically to better than half a percent except where tidal distortions are becoming extreme. We show that the differences could be interpreted as representing small residual eccentricity in the initial orbits. In comparing the diagnostic with preliminary numerical data on neutron star-black hole binaries, we find less agreement.

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The Initial Data Problem

Gourgoulhon

2012

3+1 Formalism in General Relativity

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Various features of quasiequilibrium sequences of binary neutron stars in general relativity

Cited by 63 publications

References 71 publications

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Post-Newtonian diagnosis of quasiequilibrium configurations of neutron star–neutron star and neutron star–black hole binaries

The Initial Data Problem

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