Star formation rate density and the stochastic background of gravitational waves

Araújo, J. C. N. de; Miranda, Oswaldo D.

doi:10.1103/physrevd.71.127503

Cited by 11 publications

(18 citation statements)

References 17 publications

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“…Correcting for this effect is not always straightforward. Thus, there are large uncertainties associated to the determination of the CSFR as can be seen from Figs 1–3 (see, in particular, Hopkins 2004; de Araujo & Miranda 2005 who discuss these uncertainties with more details).…”

Section: The Cosmic Star Formationmentioning

confidence: 99%

“…In this section we use the CSFR obtained from the hierarchical model to determine the stochastic background of gravitational waves (SBGWs) generated by stars which collapse to black holes. Initially, we present a quick overview on the formalism used to characterize a SBGWs because this subject is discussed in previous works (see, for example, de Araujo et al 2000, 2002, 2004; Miranda, de Araujo & Aguiar 2004; de Araujo & Miranda 2005). After this quick overview we display and compare the results of the models considered.…”

Section: The Stochastic Background Of Gravitational Wavesmentioning

confidence: 99%

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Stochastic background of gravitational waves generated by pre-galactic black holes

Pereira

Miranda

2010

Monthly Notices of the Royal Astronomical Society

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In this work, we consider the stochastic background of gravitational waves (SBGWs) produced by pre‐galactic stars, which form black holes in scenarios of structure formation. The calculation is performed in the framework of hierarchical structure formation using a Press–Schechter‐like formalism. Our model reproduces the observed star formation rate at redshifts z≲ 6.5. The signal predicted in this work is below the sensitivity of the first generation of detectors but could be detectable by the next generation of ground‐based interferometers. Specifically, correlating two coincident advanced Laser Interferometer Gravitational‐Wave Observatory (LIGO) detectors (LIGO III interferometers), the expected signal‐to‐noise ratio (S/N) could be as high as 90 (10) for stars forming at redshift z≃ 20 with a Salpeter initial mass function with slope x= 0.35 (1.35), and if the efficiency of generation of gravitational waves, namely, εGW is close to the maximum value ∼7 × 10−4. However, the sensitivity of the future third generation of detectors as, for example, the European antenna EGO could be high enough to produce S/N > 3 same with εGW∼ 2 × 10−5. We also discuss what astrophysical information could be derived from a positive (or even negative) detection of the SBGWs investigated here.

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Section: The Cosmic Star Formationmentioning

confidence: 99%

Section: The Stochastic Background Of Gravitational Wavesmentioning

confidence: 99%

Stochastic background of gravitational waves generated by pre-galactic black holes

Pereira

Miranda

2010

Monthly Notices of the Royal Astronomical Society

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“…The factor (1 + z) in equation (4) converts R(z) to an earth time based quantity. The statement that such a factor does not exist given in de Araujo & Miranda (2005) does not change the calculation of ΩGW(f ) as the factor appears additionally in their equation for dE/dSdf . This caveat has also appeared in other publications, e.g., Regimbau & Mandic (2008); Zhu et al (2010Zhu et al ( , 2011a; Howell et al (2011).…”

Section: Properties Of An Agwbmentioning

confidence: 99%

On the gravitational wave background from compact binary coalescences in the band of ground-based interferometers

Zhu¹,

Howell²,

Blair³

et al. 2013

Monthly Notices of the Royal Astronomical Society

128

115

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This paper reports a comprehensive study on the gravitational wave (GW) background from compact binary coalescences. We consider in our calculations newly available observation-based neutron star and black hole mass distributions and complete analytical waveforms that include post-Newtonian amplitude corrections. Our results show that: (i) post-Newtonian effects cause a small reduction in the GW background signal; (ii) below 100 Hz the background depends primarily on the local coalescence rate r 0 and the average chirp mass and is independent of the chirp mass distribution; (iii) the effects of cosmic star formation rates and delay times between the formation and merger of binaries are linear below 100 Hz and can be represented by a single parameter within a factor of ∼ 2; (iv) a simple power law model of the energy density parameter Ω GW (f ) ∼ f 2/3 up to 50-100 Hz is sufficient to be used as a search template for ground-based interferometers. In terms of detection prospects of this background signal, we show that: (i) detection (a signal-to-noise ratio of 3) within one year of observation by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors (H1-L1) requires a coalescence rate of r 0 = 3 (0.2) Mpc −3 Myr −1 for binary neutron stars (binary black holes); (ii) this limit on r 0 could be reduced 3-fold for two co-located and co-aligned detectors, whereas the currently proposed worldwide network of advanced instruments gives only ∼ 30% improvement in detectability; (iii) the improved sensitivity of the planned Einstein Telescope allows not only confident detection of the background but also the high frequency components of the spectrum to be measured, possibly enabling rate evolutionary histories and mass distributions to be probed. Finally we show that sub-threshold binary neutron star merger events produce a strong foreground, which could be an issue for future terrestrial stochastic searches of primordial GWs.

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“…From (1), (7) and (29), one notices that √ S h ∝ ρ * (z 0 ) and √ S h ∝ √ λ nsns . Therefore, if ones multiplyρ * (z 0 ) or λ nsns by, say, a factor of 10, the amplitudes shown in Fig.…”

Section: Resultsmentioning

confidence: 94%

“…where α = 3/5, β = 14/15, z m = 5.4 and with ρ m = 0.15M ⊙ yr −1 Mpc −3 fixing the normalization. Besides, in (7), λ nsns = β ns f p Φ ns (see [1]) is the mass fraction of stars that is converted into neutron stars, where β ns is the fraction of binaries that survive to the second supernova event; f p gives the fraction of massive binaries (that is, those systems where both components can generate supernovae) and Φ ns is the mass fraction of progenitors that originates neutron stars, which, in the present case, is calculated by…”

Section: Calculation Of Dr/dvmentioning

confidence: 98%

The Gravitational Wave Background from Coalescing Compact Binaries: A New Method

Evangelista

Araújo

2014

Braz J Phys

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Gravitational waves are perturbations in the spacetime that propagate at the speed of light. The study of such phenomenon is interesting because many cosmological processes and astrophysical objects, such as binary systems, are potential sources of gravitational radiation and can have their emissions detected in the near future by the next generation of interferometric detectors. Concerning the astrophysical objects, an interesting case is when there are several sources emitting in such a way that there is a superposition of signals, resulting in a smooth spectrum which spans a wide range of frequencies, the so-called stochastic background. In this paper, we are concerned with the stochastic backgrounds generated by compact binaries (i.e. binary systems formed by neutron stars and black holes) in the coalescing phase. In particular, we obtain such backgrounds by employing a new method developed in our previous studies.

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Star formation rate density and the stochastic background of gravitational waves

Cited by 11 publications

References 17 publications

Stochastic background of gravitational waves generated by pre-galactic black holes

Stochastic background of gravitational waves generated by pre-galactic black holes

On the gravitational wave background from compact binary coalescences in the band of ground-based interferometers

The Gravitational Wave Background from Coalescing Compact Binaries: A New Method

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