1999/02/01 by Valeria Ferrari, Sabino Matarrese, Raffaella Schneider · 5 citations
Physics and Astronomy · #Pulsars and Gravitational Waves Research #Gamma-ray bursts and supernovae #Cosmology and Gravitation Theories
paper · pdf · doi:10.1046/j.1365-8711.1999.02194.x
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, Q GW , 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.