Stochastic background of gravitational waves

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

doi:10.1103/physrevd.61.124015

Cited by 35 publications

(46 citation statements)

References 11 publications

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“…While the full three-dimensional simulations that include all relevant processes are yet to be made, predictions have already been made about the gravitationalwave signals emitted during core collapse [62][63][64]. These predictions have then been used to make estimates of the corresponding SGWB due to both standard and early (population III) stars [41,[65][66][67][68][69][70][71][72][73][74][75]. These estimates are necessarily only approximate, both because it is currently not well understood how the gravitational-wave signal depends on the progenitor stellar parameters such as the mass or spin, and because the rate of core collapse events is uncertain.…”

Section: Introductionmentioning

confidence: 99%

Model of the stochastic gravitational-wave background due to core collapse to black holes

et al. 2015

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Superposition of gravitational waves generated by astrophysical sources is expected to give rise to the stochastic gravitational-wave background. We focus on the background generated by the ring-down of black holes produced in the stellar core collapse events across the universe. We systematically study the parameter space in this model, including the most recent information about the star formation rate and about the population of black holes as a function of redshift and of metallicity. We investigate the accessibility of this gravitational wave background to the upcoming gravitational-wave detectors, such as Advanced LIGO and Einstein Telescope.PACS numbers: 95.85. Sz, 97.60.Jd, 04.25.dg, 98.80.Cq

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Section: Introductionmentioning

confidence: 99%

Model of the stochastic gravitational-wave background due to core collapse to black holes

et al. 2015

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“…For further details we refer the reader to, e.g., [5]. It is worth mentioning that concerning the star formation at high redshift, the IMF could be biased toward high-mass stars, when compared to the solar neighborhood IMF, as a result of the absence of metals [6,7].…”

Section: Initial Mass Function and The Neutron Star Massesmentioning

confidence: 99%

“…(see [11,12]). The micro-collapse produces GWs at frequency ν of the NS f-mode, and dimensionless amplitude given by [13] h N S ≃ 1 × 10…”

Section: Gravitational Wave Productionmentioning

confidence: 99%

Gravitational wave background from neutron star phase transition for a new class of equation of state

Araújo¹,

Marranghello²

2008

J. Phys.: Conf. Ser.

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Abstract. We study the generation of a stochastic gravitational wave (GW) background produced by a population of neutron stars (NSs) which go over a hadron-quark phase transition in its inner shells. We obtain, for example, that the NS phase transition, in cold dark matter scenarios, could generate a stochastic GW background with a maximum amplitude of hBG ∼ 10 −24 , in the frequency band ≃ 20 − 2000 Hz for stars forming at redshifts of up to z ≃ 20. We study the possibility of detection of this isotropic GW background by correlating signals of a pair of 'advanced' LIGO observatories. IntroductionIt is widely accepted that neutron stars (NSs) are born with fast rotating angular velocities. Due to magnetic torques, however, the NS periods could well be spun down. This spin-down causes a reduction in the centrifuge force and, consequently, the central energy density of the NSs increases. Those stars, born with densities close to that of the quark deconfinement, may undergo a phase transition forming a strange quark matter core. It is worth stressing, however, that it is not a common sense that such a transition really takes place.As a consequence of such a putative phase transition, the stars could suffer a collapse which could excite mechanical oscillations. The great amount of energy generated in this process, ∆E ∼ 10 53 ergs (∼ 0.1 M ⊙ c 2 ) [1], could be dissipated, at least partially, in the form of gravitational waves (GWs), which are studied in the present work.We adopted in the present paper the history of star formation derived by Springel & Hernquist [2], who employed hydrodynamic simulations of structure formation in a Λ cold dark matter (ΛCDM) cosmology. These authors study the history of cosmic star formation from the "dark ages", at redshift z ∼ 20, to the present.Besides the reliable history of star formation by Springel & Hernquist, we consider the role of the parameters α i=1,2 , which gives the fraction of the progenitor mass which forms the remnant NSs. We consider that the remnant mass is given as a function of the progenitor mass, namely M r = α 1 m + α 2 . Later on we justify why M r is written in this way. Recall that a given initial mass function (IMF) refers to the distribution function of the stellar progenitor mass, and also to the masses of the remnant compact objects left as a result of the stellar evolution.In the present study we have adopted a stellar generation with a Salpeter IMF, which is consistent with Springel & Hernquist, since they show that population II stars could have been formed at high redshift too. We then discuss briefly what conclusions would be drawn whether

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“…[1]). Some authors argue that there is an additional (1 + z) term in the equation for the differential rate dividinġ ρ ⋆ (z), which would take into account the effect of cosmic expansion onto the time variable.…”

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confidence: 99%

“…The first group does not include this factor dividing the SFRD (see, e.g., Refs. [1,2,3]). On the other hand, the second group argues that it is necessary to include the factor (1 + z) to account for the time dilation of the observed rate by cosmic expansion, converting a source-count equation to an event-rate equation (see, e.g., Refs.…”

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confidence: 99%

Star formation rate density and the stochastic background of gravitational waves

Araújo

Miranda

2005

Phys. Rev. D

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There is in the literature a number of papers addressing the stochastic background of gravitational waves (GWs) generated by an ensemble of astrophysical sources. The main ingredient in such studies is the so called star formation rate density (SFRD), which gives the density of stars formed per unit time. Some authors argue, however, that there is, in the equation that determines the amplitude of the stochastic background of GWs, an additional (1 + z) term dividing the SFRD, which would account for the effect of cosmic expansion onto the time variable. We argue here that the inclusion of this additional term is wrong. In order to clarify where the inclusion of the (1 + z) term is really necessary, we briefly discuss the calculation of event rates in the study of GRBs (gamma ray bursts) from cosmological origin.

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Stochastic background of gravitational waves

Cited by 35 publications

References 11 publications

Model of the stochastic gravitational-wave background due to core collapse to black holes

Model of the stochastic gravitational-wave background due to core collapse to black holes

Gravitational wave background from neutron star phase transition for a new class of equation of state

Star formation rate density and the stochastic background of gravitational waves

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