Formation of double compact objects

Kalogera, V.; Belczyński, Krzysztof; Kim, Chunglee; O’Shaughnessy, R.; Willems, Bart

doi:10.1016/j.physrep.2007.02.008

Cited by 187 publications

(199 citation statements)

References 78 publications

(142 reference statements)

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“…II made by McWilliams [1] with LISA. We do not consider BH/BH binaries with DECIGO/BBO here since these merger rates are expected to be about 1 order of magnitude smaller than the BH/NS ones [56,57]. We define N as the averaged number of detection events expected in GR and N H as the one in RS-II model.…”

Section: Constraints From the Expected Numbers Of Emri And Bh/ns mentioning

confidence: 99%

Probing the size of extra dimensions with gravitational wave astronomy

2011

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In Randall-Sundrum II (RS-II) braneworld model, it has been conjectured according to the AdS/CFT correspondence that brane-localized black hole (BH) larger than the bulk AdS curvature scale ℓ cannot be static, and it is dual to a four dimensional BH emitting the Hawking radiation through some quantum fields. In this scenario, the number of the quantum field species is so large that this radiation changes the orbital evolution of a BH binary. We derived the correction to the gravitational waveform phase due to this effect and estimated the upper bounds on ℓ by performing Fisher analyses. We found that DECIGO/BBO can put a stronger constraint than the current table-top result by detecting gravitational waves from small mass BH/BH and BH/neutron star (NS) binaries. Furthermore, DECIGO/BBO is expected to detect 10 5 BH/NS binaries per year. Taking this advantage, we found that DECIGO/BBO can actually measure ℓ down to ℓ = 0.33µm for 5 year observation if we know that binaries are circular a priori. This is about 40 times smaller than the upper bound obtained from the table-top experiment. On the other hand, when we take eccentricities into binary parameters, the detection limit weakens to ℓ = 1.5µm due to strong degeneracies between ℓ and eccentricities. We also derived the upper bound on ℓ from the expected detection number of extreme mass ratio inspirals (EMRIs) with LISA and BH/NS binaries with DECIGO/BBO, extending the discussion made recently by McWilliams [1]. We found that these less robust constraints are weaker than the ones from phase differences.

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Section: Constraints From the Expected Numbers Of Emri And Bh/ns mentioning

confidence: 99%

Probing the size of extra dimensions with gravitational wave astronomy

2011

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“…4 For large likelihood differences, all models are consistent and V converges to the whole parameter space. In practice, the simulation space cannot be exhaustively explored: not enough computing power is available to sample all possible likelihood differences.…”

Section: B Fisher Matrix and Local Dimensionalitymentioning

confidence: 99%

“…Ground-based gravitational-wave interferometric detectors like advanced LIGO and Virgo are expected to detect at least a few coalescing compact binaries (CCBs) per year, based both on semi-empirical extrapolations of Milky Way binary pulsar statistics [1][2][3] and on theoretical predictions both of isolated binary [4][5][6][7][8][9] and clustered evolution [10][11][12][13]. Each detected waveform should reveal the sky location, distance, component masses, and conceivably even component spins.…”

Section: Introductionmentioning

confidence: 99%

Data-driven methods to explore a large space of computationally costly compact binary progenitor models

O’Shaughnessy

2013

Phys. Rev. D

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Being able to measure each merger's sky location, distance, component masses, and conceivably spins, ground-based gravitational-wave detectors will provide a extensive and detailed sample of coalescing compact binaries (CCBs) in the local and, with third-generation detectors, distant universe. These measurements will distinguish between competing progenitor formation models. In this paper we develop practical tools to characterize the amount of experimentally accessible information available, to distinguish between two a priori progenitor models. Using a simple time-independent model, we demonstrate the information content scales strongly with the number of observations. The exact scaling depends on how significantly mass distributions change between similar models. We develop phenomenological diagnostics to estimate how many models can be distinguished, using first-generation and future instruments. Finally, we emphasize that multi-observable distributions can be fully exploited only with very precisely calibrated detectors, search pipelines, parameter estimation, and Bayesian model inference.

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“…According to current thinking, these binaries are formed from the individual collapse of binaries of main sequence stars [66]. If one can establish a population model for our galaxy, therefore, one should be able to deduce the population outside the galaxy by comparing the rate of star formation in our galaxy to elsewhere.…”

Section: Neutron Star Binaries As Gravitational Wave Emittersmentioning

confidence: 99%

“…Thus, there is not much information to feed into these models, and estimates can still vary widely. The current best estimate is that LIGO should now be able to observe of the order of one BNS system approximately every hundred years, although uncertainties extend this from a few per thousand years to almost one every ten years [66]. An improvement in LIGO's ability to detect BNS systems by a factor of three would therefore raise the most optimistic case to almost one BNS signal per year.…”

Section: Neutron Star Binaries As Gravitational Wave Emittersmentioning

confidence: 99%

Searches for Gravitational Waves from Binary Neutron Stars: A Review

Anderson

Creighton

2008

Astrophysics and Space Science Library

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Summary.A new generation of observatories is looking for gravitational waves. These waves, emitted by highly relativistic systems, will open a new window for observation of the cosmos when they are detected. Among the most promising sources of gravitational waves for these observatories are compact binaries in the final minutes before coalescence. In this article, we review in brief interferometric searches for gravitational waves emitted by neutron star binaries, including the theory, instrumentation and methods. No detections have been made to date. However, the best direct observational limits on coalescence rates have been set, and instrumentation and analysis methods continue to be refined toward the ultimate goal of defining the new field of gravitational wave astronomy.

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Formation of double compact objects

Cited by 187 publications

References 78 publications

Probing the size of extra dimensions with gravitational wave astronomy

Probing the size of extra dimensions with gravitational wave astronomy

Data-driven methods to explore a large space of computationally costly compact binary progenitor models

Searches for Gravitational Waves from Binary Neutron Stars: A Review

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