Bowen-York trumpet data and black-hole simulations

Hannam, M. D.; Husa, S.; Murchadha, Niall Ó

doi:10.1103/physrevd.80.124007

Cited by 45 publications

(71 citation statements)

References 58 publications

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“…The irreducible mass M irr , as approximated by the proper area of the apparent horizon, remains equal to the mass parameter M along this sequence, to within the accuracy of our code. This finding has been confirmed by research performed concurrently with ours [26], and differs from the case for wormhole data (see, for example, the analytical treatment of [24]). …”

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confidence: 72%

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Trumpet-puncture initial data for black holes

Immerman

Baumgarte

2009

Phys. Rev. D

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We propose a new approach, based on the puncture method, to construct black hole initial data in the so-called trumpet geometry, i.e. on slices that asymptote to a limiting surface of non-zero areal radius. Our approach is easy to implement numerically and, at least for non-spinning black holes, does not require any internal boundary conditions. We present numerical results, obtained with a uniform-grid finite-difference code, for boosted black holes and binary black holes. We also comment on generalizations of this method for spinning black holes.PACS numbers: 04.20. Ex, 04.25.dg, 04.70.Bw Numerical simulations of black hole spacetimes have recently experienced a dramatic breakthrough (see [1,2,3] as well as numerous later publications). Most of these simulations now adopt some variation of the BSSN formulation [4,5] together with the moving puncture [2,3] method to handle the black hole singularities.The moving-puncture method is based on a set of empirically found coordinate conditions, namely the "1+log" slicing condition for the lapse [6] and a "Γ-freezing" gauge condition for the shift [7]. As demonstrated by [8,9,10,11], dynamical simulations of a Schwarzschild spacetime using these coordinate conditions settle down to a spatial slice that terminates at a non-zero areal radius, and hence does not encounter the spacetime singularity at the center of the black hole. An embedding diagram of such a slice, which suggests the name trumpet data, is shown in Fig. 2 of [11].Typically, moving-puncture simulations adopt initial data that are constructed using the puncture method [12,13,14]. As we explain in more detail below, the central idea of the puncture method is to write the conformal factor as a sum of an analytically known, singular background term, and a correction term that is unknown but regular. The equations for the correction term can then be solved everywhere, without any need for excision or any other means of dealing with the black hole singularity. To date, all applications of this method have adopted Schwarzschild data on a slice of constant Schwarzschild time as the background solution. These data connect spatial infinity in one universe with spatial infinity in another universe; the resulting initial data therefore represent wormhole data.Clearly, it would be desirable to produce initial data that represent black holes as trumpets rather than wormholes, since otherwise moving-puncture evolutions will drive the individual black holes to a trumpet geometry. Problems with one possible approach, based on a stationary 1+log slicing in the context of the conformal thin-sandwich decomposition, were described in [15]. Recently, trumpet initial data on hyperboloidal slices using * Also at Department of Physics, University of Illinois at UrbanaChampaign, Urbana, IL 61801 an excision method were constructed in [16]. In this paper we demonstrate how such data can be produced by generalizing the puncture method, which does not require any excision or internal boundary conditions, and is very easy to imple...

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confidence: 72%

“…Given the singular behavior of u S , these solutions cannot be found with the methods discussed in this paper. One possible approach would be to scale out the r −1/2 behavior explicitly, and solve only for the remaining parts of the solution, which should then be regular everywhere (compare [26]). …”

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confidence: 99%

Trumpet-puncture initial data for black holes

Immerman

Baumgarte

2009

Phys. Rev. D

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“…Most codes in the field (including BAM and SpEC) primarily use conformally flat initial data, which limits the BH spins to a/m ∼ 0.92 [43][44][45]. There has been some work in constructing high-spin data for puncture codes like BAM [46,47], but to date no waveforms for long-term quasi-circular inspirals have been published.…”

Section: B Numerical Relativity Waveformsmentioning

confidence: 99%

Frequency-domain gravitational waves from nonprecessing black-hole binaries. I. New numerical waveforms and anatomy of the signal

et al. 2016

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In this paper we discuss the anatomy of frequency-domain gravitational-wave signals from non-precessing black-hole coalescences with the goal of constructing accurate phenomenological waveform models. We first present new numerical-relativity simulations for mass ratios up to 18, including spins. From a comparison of different post-Newtonian approximants with numerical-relativity data we select the uncalibrated SEOBNRv2 model as the most appropriate for the purpose of constructing hybrid post-Newtonian/numerical-relativity waveforms, and we discuss how we prepare time-domain and frequency-domain hybrid data sets. We then use our data together with results in the literature to calibrate simple explicit expressions for the final spin and radiated energy. Equipped with our prediction for the final state we then develop a simple and accurate mergerringdown-model based on modified Lorentzians in the gravitational wave amplitude and phase, and we discuss a simple method to represent the low frequency signal augmenting the TaylorF2 post-Newtonian approximant with terms corresponding to higher orders in the post-Newtonian expansion. We finally discuss different options for modelling the small intermediate frequency regime between inspiral and merger-ringdown. A complete phenomenological model based on the present work is presented in a companion paper [1].

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“…the Schwarzschild trumpet [13], for which both 1+log and maximal slicing is known [15][16][17]. Although puncture evolutions employ the 1+log gauge, so far most investigations of trumpet initial data beyond Schwarzschild have focussed on maximally sliced trumpets [18][19][20]. Constant mean curvature slices with trumpets were considered in [21].…”

Section: Introductionmentioning

confidence: 99%

Solving the Hamiltonian constraint for1+logtrumpets

Dietrich¹,

Brügmann²

2014

Phys. Rev. D

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The puncture method specifies black hole data on a hypersurface with the aid of a conformal rescaling of the metric that exhibits a coordinate singularity at the puncture point. When constructing puncture initial data by solving the Hamiltonian constraint for the conformal factor, the coordinate singularity requires special attention. The standard way to treat the pole singularity occurring in wormhole puncture data is not generally applicable to trumpet puncture data. We investigate a new approach based on inverse powers of the conformal factor and present numerical examples for single punctures of the wormhole and 1+log-trumpet type. Additionally, we describe a method to solve the Hamiltonian constraint for two 1+log trumpets for a given extrinsic curvature with non-vanishing trace. We investigate properties of this constructed initial data during binary black hole evolutions and find that the initial gauge dynamics is reduced.

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Bowen-York trumpet data and black-hole simulations

Cited by 45 publications

References 58 publications

Trumpet-puncture initial data for black holes

Trumpet-puncture initial data for black holes

Frequency-domain gravitational waves from nonprecessing black-hole binaries. I. New numerical waveforms and anatomy of the signal

Solving the Hamiltonian constraint for1+logtrumpets

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