Care of the infant

Aylott, Marion

doi:10.1007/978-1-137-11733-5_15

Cited by 4 publications

(5 citation statements)

References 20 publications

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“…In the past decade, the field of Numerical Relativity has made great strides in modeling D = 4 asymptotically flat spacetimes and is now able to solve strongly gravitating/highly dynamical scenarios. A considerable portion of this was driven by the goal of producing answers to guide detection and analysis strategies for gravitational wave astronomy (see [18] and references cited therein) although progress has been achieved on many fronts: gravitational waves, cosmology, fundamental studies of gravity, astrophysics, etc. For further details, we refer the reader to some reviews [19,20,21,22,23,24,25,26] and textbooks [27,28,29] on the subject.…”

Section: Challenges Aheadmentioning

confidence: 99%

NR/HEP: roadmap for the future

Cardoso

Gualtieri

Herdeiro

et al. 2012

Class. Quantum Grav.

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Abstract. Physics in curved spacetime describes a multitude of phenomena, ranging from astrophysics to high energy physics. The last few years have witnessed further progress on several fronts, including the accurate numerical evolution of the gravitational field equations, which now allows highly nonlinear phenomena to be tamed. Numerical relativity simulations, originally developed to understand strong field astrophysical processes, could prove extremely useful to understand high-energy physics processes like trans-Planckian scattering and gauge-gravity dualities. We present a concise and comprehensive overview of the state-of-the-art and important open problems in the field(s), along with guidelines for the next years. This writeup is a summary of the "NR/HEP Workshop" held in Madeira, Portugal from August 31st to September 3rd 2011.arXiv:1201.5118v1 [hep-th]

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Section: Challenges Aheadmentioning

confidence: 99%

NR/HEP: roadmap for the future

Cardoso

Gualtieri

Herdeiro

et al. 2012

Class. Quantum Grav.

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“…However, we can perform one simple test to quantify the change in gauge between the two sets of data. In wormhole data, the apparent horizons of the two black holes are located on surfaces with coordinate radii close to r ≈ m/2, where m is the mass parameter in the wormhole puncture conformal ansatz (5). For trumpet data, on the other hand, the horizon is at about r ≈ 0.78M .…”

Section: A Gauge Changesmentioning

confidence: 99%

“…Numerical solutions of the full Einstein equations for the last orbits and merger of compact binary systems are important for the developing field of gravitational-wave astronomy. In the case of black-hole binaries, long-term simulations became possible in 2005 [1,2,3], and within the last few years the field has developed to the point where the gravitational-wave (GW) signal from such systems can be calculated to essentially the required accuracy of current GW detectors [4], and work is underway to incorporate these results into GW searches [5]. However, only a small fraction of the full black-hole-binary parameter space has yet been studied [6], and its full exploration will require yet more accurate and efficient numerical simulations.…”

Section: Introductionmentioning

confidence: 99%

Bowen-York trumpet data and black-hole simulations

2009

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Type of publicationArticle (peer-reviewed) The most popular method to construct initial data for black-hole-binary simulations is the puncture method, in which compactified wormholes are given linear and angular momentum via the Bowen-York extrinsic curvature. When these data are evolved, they quickly approach a trumpet topology, suggesting that it would be preferable to use data that are in trumpet form from the outset. To achieve this, we extend the puncture method to allow the construction of Bowen-York trumpets, including an outline of an existence and uniqueness proof of the solutions. We construct boosted, spinning and binary Bowen-York puncture trumpets using a single-domain pseudospectral elliptic solver, and evolve the binary data and compare with standard wormhole-data results. We also show that for boosted trumpets the black-hole mass can be prescribed a priori, without recourse to the iterative procedure that is necessary for wormhole data.

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“…However, much further work is required to actually understand the practical implications of numerical solutions of the full Einstein equations for gravitational-wave data analysis. Indeed, first studies suggest that template banks that use numerical information can increase the reach of detectors [4,5,6], aid the calibration of search pipelines [7,8,9], and improve the estimation of parameters, such as e.g., sky location [10].…”

Section: Introductionmentioning

confidence: 99%

Gravitational-wave detectability of equal-mass black-hole binaries with aligned spins

et al. 2009

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Binary black-hole systems with spins aligned or anti-aligned to the orbital angular momentum, and which therefore do not exhibit precession effects, provide the natural ground to start detailed studies of the influence of strong-field spin effects on gravitational wave observations of coalescing binaries. Furthermore, such systems may be the preferred end-state of the inspiral of generic supermassive binary black-hole systems. In view of this, we have computed the inspiral and merger of a large set of binary systems of equal-mass black holes with spins parallel to the orbital angular momentum but otherwise arbitrary. Our attention is particularly focused on the gravitational-wave emission so as to quantify how much spin effects contribute to the signal-to-noise ratio, to the horizon distances, and to the relative event rates for the representative ranges in masses and detectors. As expected, the signal-to-noise ratio increases with the projection of the total black hole spin in the direction of the orbital momentum. We find that equal-spin binaries with maximum spin aligned with the orbital angular momentum are more than "three times as loud" as the corresponding binaries with anti-aligned spins, thus corresponding to event rates up to 30 times larger. We also consider the waveform mismatch between the different spinning configurations and find that, within our numerical accuracy, binaries with opposite spins S1 = −S2 cannot be distinguished whereas binaries with spin S1 = S2 have clearly distinct gravitationalwave emissions. Finally, we derive a simple expression for the energy radiated in gravitational waves and find that the binaries always have efficiencies E rad /M 3.6%, which can become as large as E rad /M ≃ 10% for maximally spinning binaries with spins aligned with the orbital angular momentum. These binaries are therefore among the most efficient sources of energy in the Universe.

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Care of the infant

Cited by 4 publications

References 20 publications

NR/HEP: roadmap for the future

NR/HEP: roadmap for the future

Bowen-York trumpet data and black-hole simulations

Gravitational-wave detectability of equal-mass black-hole binaries with aligned spins

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