Model of the stochastic gravitational-wave background due to core collapse to black holes

Crocker, Kyle; Mandic, V.; Regimbau, T.; Belczyński, K.; Gładysz, Wojciech; Olive, Keith A.; Prestegard, T.; Vangioni, Elisabeth

doi:10.1103/physrevd.92.063005

Cited by 35 publications

(36 citation statements)

References 118 publications

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“…This is expected to be a reasonable approximation for most predicted astrophysical sources of gravitational waves. The backgrounds expected from stellar-mass binary black holes [74], core-collapse supernovae [38], and rotating neutron stars [86][87][88], for instance, are all well-modelled by power laws in the Advanced LIGO band. It may be, however, that the stochastic background is in fact not well-described by a single power law.…”

Section: Broken Tensor Spectramentioning

confidence: 98%

“…Such events are rare, occurring at a rate between (0.6 − 10.5) × 10 −2 yr −1 [37]. The stochastic gravitational-wave background, on the other hand, is dominated by distant undetected sources, and so in principle it is possible that a CCSNe background of breathing modes could be detected before the observation of a single Galactic supernova [38,39]. However, realistic simulations of monopole emission from CCSNe predict only weak scalar emission [34].…”

Section: Extended Theories Of Gravity and Alternative Polarizatiomentioning

confidence: 99%

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Polarization-Based Tests of Gravity with the Stochastic Gravitational-Wave Background

et al. 2017

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The direct observation of gravitational waves with Advanced LIGO and Advanced Virgo offers novel opportunities to test general relativity in strong-field, highly dynamical regimes. One such opportunity is the measurement of gravitational-wave polarizations. While general relativity predicts only two tensor gravitational-wave polarizations, general metric theories of gravity allow for up to four additional vector and scalar modes. The detection of these alternative polarizations would represent a clear violation of general relativity. The LIGO-Virgo detection of the binary black hole merger GW170814 has recently offered the first direct constraints on the polarization of gravitational waves. The current generation of ground-based detectors, however, is limited in its ability to sensitively determine the polarization content of transient gravitational-wave signals. Observation of the stochastic gravitational-wave background, in contrast, offers a means of directly measuring generic gravitational-wave polarizations. The stochastic background, arising from the superposition of many individually unresolvable gravitational-wave signals, may be detectable by Advanced LIGO at design sensitivity. In this paper, we present a Bayesian method with which to detect and characterize the polarization of the stochastic background. We explore prospects for estimating parameters of the background and quantify the limits that Advanced LIGO can place on vector and scalar polarizations in the absence of a detection. Finally, we investigate how the introduction of new terrestrial detectors like Advanced Virgo aid in our ability to detect or constrain alternative polarizations in the stochastic background. We find that, although the addition of Advanced Virgo does not notably improve detection prospects, it may dramatically improve our ability to estimate the parameters of backgrounds of mixed polarization.

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Section: Broken Tensor Spectramentioning

confidence: 98%

Section: Extended Theories Of Gravity and Alternative Polarizatiomentioning

confidence: 99%

Polarization-Based Tests of Gravity with the Stochastic Gravitational-Wave Background

et al. 2017

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“…The constants ω1 = f The second contribution is from a collapse of a single star which reflects the BH birth rate. We assume, following Crocker et al (2015), that most of the energy is dissipated via the ringdown of the ℓ = 2 dominant quasi-normal mode whose frequency is given by (Echeverria 1989):…”

Section: Stochastic Gravitational Wave Backgroundmentioning

confidence: 99%

“…and we take the efficiency parameter ǫ = 10 −5 from Crocker et al (2015). We assume a constant spin parameter a = 1 for all the BHs.…”

Section: Stochastic Gravitational Wave Backgroundmentioning

confidence: 99%

Metallicity-constrained merger rates of binary black holes and the stochastic gravitational wave background

Dvorkin

Vangioni

Silk

et al. 2016

Mon. Not. R. Astron. Soc.

116

133

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The recent detection of the binary black hole merger GW150914 demonstrates the existence of black holes more massive than previously observed in X-ray binaries in our Galaxy. This article explores different scenarios of black hole formation in the context of self-consistent cosmic chemical evolution models that simultaneously match observations of the cosmic star formation rate, optical depth to reionization and metallicity of the interstellar medium. This framework is used to calculate the mass distribution of merging black hole binaries and its evolution with redshift. We also study the implications of the black hole mass distribution for the stochastic gravitational wave background from mergers and from core collapse events.

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“…GW background from stellar-mass BBH is expected to be detected by Advanced LIGO [5], while the signal from SMBH is beginning to be constrained by PTA experiments and will be further probed by the eLISA satellite [7,8]. Finally, the GW signal from SN collapse is difficult to estimate due to uncertainties in the collapse mechanism [19][20][21].…”

Section: Introductionmentioning

confidence: 99%

Synthetic model of the gravitational wave background from evolving binary compact objects

et al. 2016

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Modeling the stochastic gravitational wave background from various astrophysical sources is a key objective in view of upcoming observations with ground-and space-based gravitational wave observatories such as Advanced LIGO, VIRGO, eLISA and PTA. We develop a synthetic model framework that follows the evolution of single and binary compact objects in an astrophysical context. We describe the formation and merger rates of binaries, the evolution of their orbital parameters with time and the spectrum of emitted gravitational waves at different stages of binary evolution. Our approach is modular and allows us to test and constrain different ingredients of the model, including stellar evolution, black hole formation scenarios and the properties of binary systems. We use this framework in the context of a particularly well-motivated astrophysical setup to calculate the gravitational wave background from several types of sources, including inspiraling stellar-mass binary black holes that have not merged during a Hubble time. We find that this signal, albeit weak, has a characteristic shape that can help constrain the properties of binary black holes in a way complementary to observations of the background from merger events. We discuss possible applications of our framework in the context of other gravitational wave sources, such as supermassive black holes.

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Model of the stochastic gravitational-wave background due to core collapse to black holes

Cited by 35 publications

References 118 publications

Polarization-Based Tests of Gravity with the Stochastic Gravitational-Wave Background

Polarization-Based Tests of Gravity with the Stochastic Gravitational-Wave Background

Metallicity-constrained merger rates of binary black holes and the stochastic gravitational wave background

Synthetic model of the gravitational wave background from evolving binary compact objects

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