Finite element computation of the gravitational radiation emitted by a pointlike object orbiting a nonrotating black hole

Sopuerta, Carlos F.; Laguna, Pablo

doi:10.1103/physrevd.73.044028

Cited by 51 publications

(93 citation statements)

References 73 publications

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“…Our purpose is to provide a quick reference for the extreme-mass ratio limit of numerical relativity simulations, to be compared with present and future numerical relativity calculations of binaries with large mass ratio (and possibly spin). Research in this direction is already under way: for example, evolutions of large mass ratio binaries using finite element methods can be found in [48]. The kick velocity accumulated after plunge using the 2PN and 3PN definitions of the ISCO is compared against the corresponding estimates by Blanchet et al [20] (BQW in the legend).…”

Section: Appendix C: Multipolar Distribution Of Radiation For Extremementioning

confidence: 99%

Inspiral, merger, and ringdown of unequal mass black hole binaries: A multipolar analysis

Berti¹,

et al. 2007

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We study the inspiral, merger and ringdown of unequal mass black hole binaries by analyzing a catalogue of numerical simulations for seven different values of the mass ratio (from q = M2/M1 = 1 to q = 4). We compare numerical and Post-Newtonian results by projecting the waveforms onto spin-weighted spherical harmonics, characterized by angular indices (l , m). We find that the PostNewtonian equations predict remarkably well the relation between the wave amplitude and the orbital frequency for each (l , m), and that the convergence of the Post-Newtonian series to the numerical results is non-monotonic. To leading order the total energy emitted in the merger phase scales like η 2 and the spin of the final black hole scales like η, where η = q/(1 + q) 2 is the symmetric mass ratio. We study the multipolar distribution of the radiation, finding that odd-l multipoles are suppressed in the equal mass limit. Higher multipoles carry a larger fraction of the total energy as q increases. We introduce and compare three different definitions for the ringdown starting time. Applying linear estimation methods (the so-called Prony methods) to the ringdown phase, we find resolution-dependent time variations in the fitted parameters of the final black hole. By crosscorrelating information from different multipoles we show that ringdown fits can be used to obtain precise estimates of the mass and spin of the final black hole, which are in remarkable agreement with energy and angular momentum balance calculations.

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Section: Appendix C: Multipolar Distribution Of Radiation For Extremementioning

confidence: 99%

Inspiral, merger, and ringdown of unequal mass black hole binaries: A multipolar analysis

Berti¹,

et al. 2007

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“…Sopuerta et al proposed the use of finite-element methods for an effective treatment of the particle in 2+1D. This idea was implemented so far only in a 1+1D context [31,32], and it awaits further development. Most recently, Barack and Golbourn [33] proposed a "puncture" scheme (further discussed below) for dealing with the singular behavior of the field in 2+1D.…”

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confidence: 99%

m-mode regularization scheme for the self-force in Kerr spacetime

2007

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We present a new, simple method for calculating the scalar, electromagnetic, and gravitational self forces acting on particles in orbit around a Kerr black hole. The standard "mode-sum regularization" approach for self-force calculations relies on a decomposition of the full (retarded) perturbation field into multipole modes, followed by the application of a certain mode-by-mode regularization procedure. In recent years several groups have developed numerical codes for calculating black hole perturbations directly in 2+1 dimensions (i.e., decomposing the azimuthal dependence into mmodes, but refraining from a full multipole decomposition). Here we formulate a practical scheme for constructing the self force directly from the 2+1-dimensional m-modes. While the standard mode-sum method is serving well in calculations of the self force in Schwarzschild geometry, the new scheme should allow a more efficient treatment of the Kerr problem.

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“…The main conclusion of this numerical experiment was that the use of adaptive techniques for the description of EMRIs can significantly improve the efficiency and accuracy of the numerical computations. Second, Finite Element methods have also been used to compute the perturbations generated by a particle orbiting a non-rotating BH in the Regge-Wheeler gauge [38]. In this work, it was shown how Finite Element methods can produce discretizations of the Dirac delta distributions (and their derivatives) present in the perturbative master equations and yield very accurate results for computations of GW fluxes of energy and angular momentum for all type of orbits.…”

Section: Pos(supernova)026mentioning

confidence: 99%

Gravitational Radiation from Neutron Stars and Black Holes

Fernandez-Sopuerta¹

2008

Proceedings of Supernovae: Lights in the Darkness — PoS(SUPERNOVA)

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Gravitational Wave Astronomy is becoming a reality as Earth-based interferometric gravitationalwave detectors reach the design sensitivities and move towards advanced configurations that may lead to gravitational-wave detections in the immediate future. In this contribution, I briefly summarize the basic characteristics of this new area, the discovery prospects and the potential for fundamental physics. Then, I present results of some investigations of two different sources of gravitational waves that are potential targets for present and future planned observatories. First, I will discuss the generation of gravitational radiation by non-linear effects arising from the coupling between radial and non-radial oscillations of neutron stars, which may produce distinctive gravitational-wave signatures. The gravitational radiation emitted by these sources is in the frequency band of Earth-based detectors. And second, I will discuss the gravitational-wave emission during the inspiral of extreme-mass-ratio compact binaries. In this case, the gravitational waves have low frequencies, inside the frequency band of space observatories like LISA.

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Finite element computation of the gravitational radiation emitted by a pointlike object orbiting a nonrotating black hole

Cited by 51 publications

References 73 publications

Inspiral, merger, and ringdown of unequal mass black hole binaries: A multipolar analysis

Inspiral, merger, and ringdown of unequal mass black hole binaries: A multipolar analysis

m-mode regularization scheme for the self-force in Kerr spacetime

Gravitational Radiation from Neutron Stars and Black Holes

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