Quasiequilibrium black hole-neutron star binaries in general relativity

@article{Taniguchi2007QuasiequilibriumBH,
  title={Quasiequilibrium black hole-neutron star binaries in general relativity},
  author={K eisuke Taniguchi and Thomas W. Baumgarte and Joshua A. Faber and Stuart L. Shapiro},
  journal={Physical Review D},
  year={2007},
  volume={75},
  pages={084005}
}
We construct quasiequilibrium sequences of black hole-neutron star binaries in general relativity. We solve Einstein's constraint equations in the conformal thin-sandwich formalism, subject to black hole boundary conditions imposed on the surface of an excised sphere, together with the relativistic equations of hydrostatic equilibrium. In contrast to our previous calculations we adopt a flat spatial background geometry and do not assume extreme mass ratios. We adopt a {gamma}=2 polytropic… 

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References

SHOWING 1-10 OF 102 REFERENCES

Black hole-neutron star binaries in general relativity: Quasiequilibrium formulation

We present a new numerical method for the construction of quasiequilibrium models of black hole-neutron star binaries. We solve the constraint equations of general relativity, decomposed in the

Black hole-neutron star binaries in general relativity: Effects of neutron star spin

We present new sequences of general relativistic, quasiequilibrium black hole-neutron star binaries. We solve for the gravitational field in the conformal thin-sandwich decomposition of Einstein's

Dynamical evolution of black hole-neutron star binaries in general relativity: Simulations of tidal disruption

We calculate the first dynamical evolutions of merging black hole-neutron star binaries that construct the combined black hole-neutron star spacetime in a general relativistic framework. We treat the

Merger of black hole-neutron star binaries : Nonspinning black hole case

The result indicates that the system of a BH and a massive disk of {approx}M{sub {center_dot}} is not formed from nonspinning BH-NS binaries, although a disk of mass 0.1M{ sub { center_dot} is a possible outcome.

Numerical evolutions of a black hole-neutron star system in full general relativity: Head-on collision

We present the first simulations in full general relativity of the head-on collision between a neutron star and a black hole of comparable mass. These simulations are performed through the solution

Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing

Three-dimensional simulations for the merger of binary neutron stars are performed in the framework of full general relativity. We pay particular attention to the black hole formation case and to the

Accretion dynamics in neutron star black hole binaries

We perform three-dimensional, Newtonian hydrodynamic simulations with a nuclear equation of state to investigate the accretion dynamics in neutron star black hole systems. We find as a general result

Mergers of irrotational neutron star binaries in conformally flat gravity

We present the first results from our new general relativistic, Lagrangian hydrodynamics code, which treats gravity in the conformally flat (CF) limit. The evolution of fluid configurations is

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

Quasiequilibrium sequences of binary neutron stars are numerically calculated in the framework of the Isenberg-Wilson-Mathews (IWM) approximation of general relativity. The results are presented for

Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. III. Identical and different mass stars with γ = 2

We present the first computations of quasiequilibrium binary neutron stars with different mass components in general relativity, within the Isenberg-Wilson-Mathews approximation. We consider both
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