Three-dimensional simulations of distorted black holes: Comparison with axisymmetric results

Camarda, Karen; Seidel, Edward

doi:10.1103/physrevd.59.064019

Cited by 33 publications

(55 citation statements)

References 49 publications

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“…and G m which can be obtained from any numerical spacetime by projecting out the Schwarzschild or Minkowski background [86]. For example, the coefficient H m 2 can be obtained via…”

Section: B the Regge-wheeler-zerilli-moncrief Formalismmentioning

confidence: 99%

Gravitational wave extraction in simulations of rotating stellar core collapse

et al. 2011

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We perform simulations of general relativistic rotating stellar core collapse and compute the gravitational waves (GWs) emitted in the core bounce phase of three representative models via multiple techniques. The simplest technique, the quadrupole formula (QF), estimates the GW content in the spacetime from the mass quadrupole tensor only. It is strictly valid only in the weakfield and slow-motion approximation. For the first time, we apply GW extraction methods in core collapse that are fully curvature-based and valid for strongly radiating and highly relativistic sources. These techniques are not restricted to weak-field and slow-motion assumptions. We employ three extraction methods computing (i) the Newman-Penrose (NP) scalar Ψ4, (ii) Regge-Wheeler-ZerilliMoncrief (RWZM) master functions, and (iii) Cauchy-Characteristic Extraction (CCE) allowing for the extraction of GWs at future null infinity, where the spacetime is asymptotically flat and the GW content is unambiguously defined. The latter technique is the only one not suffering from residual gauge and finite-radius effects. All curvature-based methods suffer from strong non-linear drifts. We employ the fixed-frequency integration technique as a high-pass waveform filter. Using the CCE results as a benchmark, we find that finite-radius NP extraction yields results that agree nearly perfectly in phase, but differ in amplitude by ∼ 1 − 7% at core bounce, depending on the model. RWZM waveforms, while in general agreeing in phase, contain spurious high-frequency noise of comparable amplitudes to those of the relatively weak GWs emitted in core collapse. We also find remarkably good agreement of the waveforms obtained from the QF with those obtained from CCE. The results from QF agree very well in phase and systematically underpredict peak amplitudes by ∼ 5−11%, which is comparable to the NP results and is certainly within the uncertainties associated with core collapse physics.

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“…and G m which can be obtained from any numerical spacetime by projecting out the Schwarzschild or Minkowski background [86]. For example, the coefficient H m 2 can be obtained via…”

Section: B the Regge-wheeler-zerilli-moncrief Formalismmentioning

confidence: 99%

Gravitational wave extraction in simulations of rotating stellar core collapse

et al. 2011

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“…As an alternative to ψ 4 , we also measure waves by evaluating the Zerilli-Moncrief variables, assuming the spacetime metric at large radius from the source to be representable as perturbations of a fixed Schwarzschild background [61][62][63]. We evaluate 1st-order gauge invariant odd-parity and even parity multipoles, (Q × lm and Q + lm , respectively) [64,65].…”

Section: E the Cauchy Evolution Code And Finite Radius Measurementsmentioning

confidence: 99%

Characteristic extraction in numerical relativity: binary black hole merger waveforms at null infinity

Reisswig¹,

Bishop²,

Pollney³

et al. 2010

Class. Quantum Grav.

146

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The accurate modeling of gravitational radiation is a key issue for gravitational wave astronomy. As simulation codes reach higher accuracy, systematic errors inherent in current numerical relativity waveextraction methods become evident, and may lead to a wrong astrophysical interpretation of the data. In this paper, we give a detailed description of the Cauchy-characteristic extraction technique applied to binary black hole inspiral and merger evolutions to obtain gravitational waveforms that are defined unambiguously, that is, at future null infinity. By this method we remove finite-radius approximations and the need to extrapolate data from the near zone. Further, we demonstrate that the method is free of gauge effects and thus is affected only by numerical error. Various consistency checks reveal that energy and angular momentum are conserved to high precision and agree very well with extrapolated data. In addition, we revisit the computation of the gravitational recoil and find that finite radius extrapolation very well approximates the result at J + . However, the (non-convergent) systematic differences to extrapolated data are of the same order of magnitude as the (convergent) discretisation error of the Cauchy evolution hence highlighting the need for correct wave-extraction.

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“…Here we use a gauge-invariant approach, in which the numerical spacetime is matched to perturbations of a Schwarzschild black hole (see Refs. [68][69][70]). Because our numerical grid for the evolution does not extent to spacial infinity, we have to measure the gravitational-wave content at a finite distance from the final black hole.…”

Section: Gravitational-wave Emissionmentioning

confidence: 99%

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

Löffler

Rezzolla²,

Ansorg³

2006

Phys. Rev. D

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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 of the Einstein equations combined with an accurate solution of the relativistic hydrodynamics equations via high-resolution shock-capturing techniques. The initial data is obtained by following the YorkLichnerowicz conformal decomposition with the assumption of time symmetry. Unlike other relativistic studies of such systems, no limitation is set for the mass ratio between the black hole and the neutron star, nor on the position of the black hole, whose apparent horizon is entirely contained within the computational domain. The latter extends over 400M and is covered with six levels of fixed mesh refinement. Concentrating on a prototypical binary system with mass ratio 6, we find that although a tidal deformation is evident the neutron star is accreted promptly and entirely into the black hole. While the collision is completed before 300M, the evolution is carried over up to 1700M, thus providing time for the extraction of the gravitational-wave signal produced and allowing for a first estimate of the radiative efficiency of processes of this type.

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Three-dimensional simulations of distorted black holes: Comparison with axisymmetric results

Cited by 33 publications

References 49 publications

Gravitational wave extraction in simulations of rotating stellar core collapse

Gravitational wave extraction in simulations of rotating stellar core collapse

Characteristic extraction in numerical relativity: binary black hole merger waveforms at null infinity

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

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