Radial Distribution of GRBs in Host Galaxies

Kosenko, D.; Блинников, С. И.; Постнов, К. А.; Bartunov, O. S.

doi:10.1007/1-4020-3748-1_9

Cited by 13 publications

(24 citation statements)

References 5 publications

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“…The implication of the evolving galaxy population has been investigated by Kosenko & Postnov (1998) in order to estimate the stochastic gravitational background produced by extragalactic merging binary white dwarfs. They show that when the global SFR evolution is included, the level of this extragalactic background can be comparable with the corresponding galactic background signal.…”

Section: The Rate Of Black Hole Collapsementioning

confidence: 99%

“…A strategy for detecting these signals with one interferometric antenna, by squaring the detector amplitude and searching for a sidereal modulation, has been proposed in Giazotto, Bonazzola & Gourgoulhon (1997) and Giampieri (1997). Further studies have estimated the intensity of the stochastic background produced by the galactic merging of unresolved binary white dwarfs (Postnov 1997), and have subsequently extended to the merging of extragalactic white dwarfs for different cosmological models (Kosenko & Postnov 1998). The considered range of frequency is 10 −3 −10 −2 Hz .…”

Section: Introductionmentioning

confidence: 99%

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Gravitational wave background from a cosmological population of core-collapse supernovae

Ferrari¹,

Matarrese²,

Schneider³

1999

Monthly Notices of the Royal Astronomical Society

135

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We analyse the stochastic background of gravitational radiation emitted by a cosmological population of core‐collapse supernovae. The supernova rate as a function of redshift is deduced from an observation‐based determination of the star formation rate density evolution. We then restrict our analysis to the range of progenitor masses leading to black hole collapse. In this case, the main features of the gravitational wave emission spectra have been shown to be, to some extent, independent of the initial conditions and of the equation of state of the collapsing star, and to depend only on the black hole mass and angular momentum. We calculate the overall signal produced by the ensemble of black hole collapses throughout the Universe, assuming a flat cosmology with a vanishing cosmological constant. Within a wide range of parameter values, we find that the spectral strain amplitude has a maximum at a few hundred Hz with an amplitude between 10‐28 and 10‐27 Hz‐1/2; the corresponding closure density, ΩGW, has a maximum amplitude ranging between 10‐11 and 10‐10 in the frequency interval ∼ 1.5‐2.5 kHz. Contrary to previous claims, our observation‐based determination leads to a duty cycle of order 0.01, making our stochastic background a non‐continuous one. Although the amplitude of our background is comparable to the sensitivity that can be reached by a pair of advanced LIGO detectors, the characteristic shot‐noise structure of the predicted signal might, in principle, be exploited to design specific detection strategies.

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Section: The Rate Of Black Hole Collapsementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gravitational wave background from a cosmological population of core-collapse supernovae

Ferrari¹,

Matarrese²,

Schneider³

1999

Monthly Notices of the Royal Astronomical Society

135

View full text Add to dashboard Cite

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“…Hils et al (1990) made detailed estimates of the Galactic binary background, and estimated that the extragalactic background from close double white dwarf pairs should be about 2 per cent (in flux or Ω units) of the Galactic background. This estimate was refined, using more modern star formation histories, by Kosenko & Postnov (1998), who found instead a level of ∼10 per cent. Schneider et al (2001) used a descendant of the Utrecht population synthesis code to estimate the extragalactic binary background as a function of frequency, and claimed that the background should have a large peak at ∼3 × 10 −5 Hz, just below the frequency at which typical binaries have a lifetime that equals the age of the Universe.…”

Section: Introductionmentioning

confidence: 99%

The gravitational wave background from cosmological compact binaries

Farmer

Phinney

2003

Monthly Notices of the Royal Astronomical Society

312

361

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We use a population synthesis approach to characterize, as a function of cosmic time, the extragalactic close binary population descended from stars of low to intermediate initial mass. The unresolved gravitational wave (GW) background due to these systems is calculated for the 0.1–10 mHz frequency band of the planned Laser Interferometer Space Antenna (LISA). This background is found to be dominated by emission from close white dwarf–white dwarf (WD–WD) pairs. The spectral shape can be understood in terms of some simple analytic arguments. To quantify the astrophysical uncertainties, we construct a range of evolutionary models which produce populations consistent with Galactic observations of close WD–WD binaries. The models differ in binary evolution prescriptions as well as initial parameter distributions and cosmic star formation histories. We compare the resulting background spectra, the shapes of which are found to be insensitive to the model chosen, and different to those found recently by Schneider et al. From this set of models, we constrain the amplitude of the extragalactic background to be 1 × 10−12≲Ωgw(1 mHz) ≲ 6 × 10−12, in terms of Ωgw( f), the fraction of closure density received in gravitational waves in the logarithmic frequency interval around f.

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“…Nelemans et al 2001). At frequencies below 10 −3 Hz, the stochastic background formed by unresolved galactic binaries is expected to be significant and be larger in amplitude when compared with both the LISA detector noise and the extragalactic background formed by merging white dwarfs (Hils et al 1990; Kosenko & Postnov 1998; Hiscock et al 2000; Nelemans et al 2001). As discussed in Seto & Cooray (2004, also, Ungarelli & Vecchio 2001), this galactic background of gravitational waves is highly anisotropic as it is mostly concentrated towards the galactic plane and the bulge.…”

Section: Introductionmentioning

confidence: 99%

Gravitational-wave background of neutron star-white dwarf binaries

Cooray

2004

Monthly Notices of the Royal Astronomical Society

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We discuss the stochastic background of gravitational waves from ultra‐compact neutron star–white dwarf (NS–WD) binaries at cosmological distances. Under the assumption that accreting neutron stars and donor white dwarf stars form most of the low‐mass X‐ray binaries (LMXBs), our calculation makes use of recent results related to the luminosity function determined from X‐ray observations. Even after accounting for detached NS–WD binaries not captured in X‐ray data, the NS–WD background is at least an order of magnitude below that due to extragalactic white dwarf–white dwarf binaries and below the detectability level of the Laser Interferometer Space Antenna (LISA) at frequencies between 10−5 and 10−1 Hz. While the extragalactic background is unlikely to be detected, we suggest that around one to 10 galactic NS–WD binaries may be resolved with LISA such that their positions are determined to an accuracy of several degrees on the sky.

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Radial Distribution of GRBs in Host Galaxies

Cited by 13 publications

References 5 publications

Gravitational wave background from a cosmological population of core-collapse supernovae

Gravitational wave background from a cosmological population of core-collapse supernovae

The gravitational wave background from cosmological compact binaries

Gravitational-wave background of neutron star-white dwarf binaries

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