Black-hole puncture initial data with realistic gravitational wave content

Kelly, Bernard; Tichy, Wolfgang; Campanelli, Manuela; Whiting, B. F.

doi:10.1103/physrevd.76.024008

Cited by 45 publications

(60 citation statements)

References 51 publications

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“…It is sufficient to use 2PN estimates because standard puncture data are inconsistent with PN theory beyond (v/c) 3 [16,17,18,19]. These parameters along with the initial ADM mass M i and angular momentum J i are shown in Table I.…”

Section: Numerical Techniques and Testsmentioning

confidence: 99%

High-spin binary black hole mergers

Marronetti

Tichy

Brügmann³

et al. 2008

Phys. Rev. D

179

219

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We study identical mass black hole binaries with spins perpendicular to the binary's orbital plane. These binaries have individual spins ranging from s/m 2 = −0.90 to 0.90, (s1 = s2 in all cases) which is near the limit possible with standard Bowen-York puncture initial data. The extreme cases correspond to the largest initial spin simulations to date. Our results expand the parameter space covered by Rezzolla et al. and, when combining both data sets, we obtain estimations for the minimum and maximum values for the intrinsic angular momenta of the remnant of binary black hole mergers of J/M 2 = 0.341 ± 0.004 and 0.951 ± 0.004 respectively. Note, however, that these values are reached through extrapolation to the singular cases |s1| = |s2| = 1 and thus remain as estimates until full-fledged numerical simulations provide confirmation.

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Section: Numerical Techniques and Testsmentioning

confidence: 99%

High-spin binary black hole mergers

Marronetti

Tichy

Brügmann³

et al. 2008

Phys. Rev. D

179

219

View full text Add to dashboard Cite

show abstract

“…Apart from this initial burst, there appears to be no unphysical behavior associated with conformally flat initial data, and this choice remains popular (See Refs. [48,49] for more astrophysically realistic initial data using post-Newtonian information). The simplest initial data, Bowen-York (BY), gives the extrinsic curvature, K ij analytically by assuming that it is transverse and traceless (See [50] for an alternative prescription).…”

Section: Introductionmentioning

confidence: 99%

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

2008

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We evolve equal-mass, equal-spin black-hole binaries with specific spins of a/mH ∼ 0.925, the highest spins simulated thus far and nearly the largest possible for Bowen-York black holes, in a set of configurations with the spins counter-aligned and pointing in the orbital plane, which maximizes the recoil velocities of the merger remnant, as well as a configuration where the two spins point in the same direction as the orbital angular momentum, which maximizes the orbital hang-up effect and remnant spin. The coordinate radii of the individual apparent horizons in these cases are very small and the simulations require very high central resolutions (h ∼ M/320). We find that these highly spinning holes reach a maximum recoil velocity of ∼ 3300 km s −1 (the largest simulated so far) and, for the hangup configuration, a remnant spin of a/mH ∼ 0.922. These results are consistent with our previous predictions for the maximum recoil velocity of ∼ 4000 km s −1 and remnant spin; the latter reinforcing the prediction that cosmic censorship is not violated by merging highlyspinning black-hole binaries. We also numerically solve the initial data for, and evolve, a single maximal-Bowen-York-spin black hole, and confirm that the 3-metric has an O(r −2 ) singularity at the puncture, rather than the usual O(r −4 ) singularity seen for non-maximal spins.

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“…They also reduce to the corotating limit (where V i = 0) as is evident from Eqs. (42) and (46) which are written in terms of V i . Furthermore, our equations reduce to the correct Newtonian limit.…”

Section: Discussionmentioning

confidence: 99%

“…choosing a post-Newtonian expression forγ ij or by matching a post-Newtonian metric with a single neutron star solution similar to [43][44][45][46][47][48]. Using Eq.…”

Section: F Further Simplifications and Boundary Conditionsmentioning

confidence: 99%

Initial data for binary neutron stars with arbitrary spins

Tichy

2011

Phys. Rev. D

137

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In general neutron stars in binaries are spinning. Due to the existence of millisecond pulsars we know that these spins can be substantial. We argue that spins with periods on the order a few dozen milliseconds could influence the late inspiral and merger dynamics. Thus numerical simulations of the last few orbits and the merger should start from initial conditions that allow for arbitrary spins. We discuss quasi-equilibrium approximations one can make in the construction of binary neutron star initial data with spins. Using these approximations we are able to derive two new matter equations. As in the case of irrotational neutron star binaries one of these equations is algebraic and the other elliptic. If these new matter equations are solved together with the equations for the metric variables following the Wilson-Mathews or conformal thin sandwich approach one can construct neutron star initial data. The spin of each star is described by a rotational velocity that can be chosen freely so that one can create stars in arbitrary rotation states. Our new matter equations reduce to the well known limits of both corotating and irrotational neutron star binaries.

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Black-hole puncture initial data with realistic gravitational wave content

Cited by 45 publications

References 51 publications

High-spin binary black hole mergers

High-spin binary black hole mergers

Extra-large remnant recoil velocities and spins from near-extremal-Bowen-York-spin black-hole binaries

Initial data for binary neutron stars with arbitrary spins

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