@Article{Miranda:2012:RoDaEn,
author = "Miranda, Oswaldo Duarte",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)}",
title = "Stochastic backgrounds of gravitational waves from cosmological
sources - the role of dark energy",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2012",
volume = "426",
number = "4",
pages = "2758--2771",
month = "Nov.",
keywords = "close binaries, dark energy, gravitational waves, large-scale
structure of universe, neutron stars.",
abstract = "In this work we investigate the detectability of the gravitational
stochastic background produced by cosmological sources in
scenarios of structure formation. The calculation is performed in
the framework of hierarchical structure formation using a
Press-Schechter-like formalism. The model considers the
coalescences of three kinds of binary systems, namely double
neutron stars (NS-NS), the neutron star-black hole (NS-BH)
binaries and the black hole-black hole (BH-BH) systems. We also
included in the model the core-collapse supernovae leaving black
holes as compact remnants. In particular, we use two different
dark energy scenarios, specifically cosmological constant
(\Λ) and Chaplygin gas, in order to verify their influence
on the cosmic star formation rate, the coalescence rates and the
gravitational wave backgrounds. We calculate the gravitational
wave signals separately for each kind of source and also determine
their collective contribution for the stochastic background of
gravitational waves. Concerning the compact binary systems, we
verify that these sources produce stochastic backgrounds with
signal-to-noise ratio (S/N) values \∼1.5 (\∼0.90)
for NS-NS, \∼0.50 (\∼0.30) for NS-BH, \∼0.20
(\∼0.10) for BH-BH and \∼0.14 (\∼0.07) for
core-collapse supernovae for a pair of advanced LIGO detectors in
the cosmological-constant (Chaplygin gas) cosmology. Particularly,
the sensitivity of the future third-generation detectors such as
the Einstein Telescope (ET), in the triangular configuration,
could increase the present S/N values by a high factor
(\∼300-1000) when compared to the S/N calculated for
advanced LIGO detectors. As an example, the collective
contribution of these sources can produce S/N \∼ 3.3
(\∼1.8) for the \Λ (Chaplygin gas) cosmology for a
pair of advanced LIGO interferometers and within the frequency
range \∼10Hz-1.5kHz. Considering ET we have S/N \∼
2200 (\∼1300) for the \Λ (Chaplygin gas) cosmology.
Thus, the third-generation gravitational wave detectors could be
used to reconstruct the history of star formation in the Universe
and to contribute for the characterization of the dark energy, for
example, identifying if there is evidence for the evolution of the
dark energy equation-of-state parameter w(a).",
doi = "10.1111/j.1365-2966.2012.21887.x",
url = "http://dx.doi.org/10.1111/j.1365-2966.2012.21887.x",
issn = "1365-2966",
label = "lattes: 9527086189389353 1 Miranda:2012:RoDaEn",
language = "en",
targetfile = "mnr21887.pdf",
urlaccessdate = "05 jun. 2024"
}