Adiabatic string shape for nonuniform rotation

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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“…Since some authors use, instead of GW , the gravitational strain S 1/2 h , defined by Allen & Romano (1999) as…”

Section: T H E S To C H a S T I C Bac K G Ro U N D O F G R Av I Tat Imentioning

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 most promising detection strategy for continuous GW background signals is cross-correlating the output of two neighbouring detectors (see Maggiore 2000;Allen & Romano 1999). For this strategy to be achieved, the detectors must be separated by less than one reduced wavelength, which is about 100 km for frequencies around 500 Hz where B (f ) might peak.…”

Section: E T E C T I O Nmentioning

confidence: 99%

Gravitational wave background from sub-luminous GRBs: prospects for second- and third-generation detectors

Howell¹,

Regimbau²,

Corsi³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We assess the detection prospects of a gravitational wave background associated with sub‐luminous gamma‐ray bursts (SL‐GRBs). We assume that the central engines of a significant proportion of these bursts are provided by newly born magnetars and consider two plausible GW emission mechanisms. First, the deformation‐induced triaxial GW emission from a newly born magnetar. Secondly, the onset of a secular bar‐mode instability, associated with the long‐lived plateau observed in the X‐ray afterglows of many gamma‐ray bursts. With regards to detectability, we find that the onset of a secular instability is the most optimistic scenario: under the hypothesis that SL‐GRBs associated with secularly unstable magnetars occur at a rate of (48–80) Gpc−3 yr−1 or greater, cross‐correlation of data from two Einstein Telescopes (ETs) could detect the GW background associated to this signal with a signal‐to‐noise ratio of 3 or greater after 1 year of observation. Assuming neutron star spindown results purely from triaxial GW emissions, we find that rates of around (130–350) Gpc−3 yr−1 will be required by ET to detect the resulting GW background. We show that a background signal from secular instabilities could potentially mask a primordial GW background signal in the frequency range where ET is most sensitive. Finally, we show how accounting for cosmic metallicity evolution can increase the predicted signal‐to‐noise ratio for background signals associated with SL‐GRBs.

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“…The most promising detection strategy is that of cross-correlation of the output of two neighbouring detectors, as reviewed by Allen & Romano (1999) and Maggiore (2000). For the signals in them to be correlated, the detectors must be separated by less than one reduced wavelength, which is about 100 km for frequencies around 500 Hz where B (f ) might peak.…”

Section: E T E C Ta B I L I T Ymentioning

confidence: 99%

The gravitational wave background from neutron star birth throughout the cosmos

Howell

Coward

Burman

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present calculations of the stochastic gravitational wave (GW) background resulting from neutron star birth throughout the Universe. We update previous calculations by employing three GW waveforms from Dimmelmeier, Font & Müller, based on three models incorporating general relativistic effects for the axisymmetric core collapse of rotating massive stars. Source‐rate evolution is accounted for by using a simulated star formation rate model based on a ‘flat‐Λ’ cosmology given by Hernquist & Springel. We show that the GW background is only weakly dependent on the source‐rate evolution model. Prominent features in the single‐source GW spectral strain can be related to the calculated background spectra, even though the features are broadened and redshifted because of contributions from high‐redshift sources. The background spectral closure density is reduced by 1–2 orders of magnitude compared with previous calculations, a consequence of using relativistic single‐source GW waveforms and a more slowly evolving source‐rate density. Duty cycle estimates for this background imply a non‐continuous signal, assuming that it consists predominantly of ‘regular’ and ‘rapid’ core‐collapse models. We note that the background may be considerably enhanced by the inclusion of dynamic post‐collapse instabilities (bar modes), which are not included in this work, so our estimates for this background may be lower limits.

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Adiabatic string shape for nonuniform rotation

Cited by 107 publications

References 7 publications

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

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

Gravitational wave background from sub-luminous GRBs: prospects for second- and third-generation detectors

The gravitational wave background from neutron star birth throughout the cosmos

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