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Cosmic Background of Gravitational Waves from Rotating Neutron Stars
Astrophysics · Submitted 15 May 2001
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim For an equatorial ellipticity of $\epsilon$ = 10$^{-6}$, the equivalent density parameter due to gravitational waves has a maximum amplitude in the range 2$\times10^{-11}-3\times10^{-9}$, around 0.9-1.5 kHz.
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The abstract, sentence by sentence
The extragalactic background of gravitational waves produced by tri-axial rotating neutron stars was calculated, under the assumption that the properties of the underlying pulsar population are the same of those of the galactic population, recently derived by Regimbau & de Freitas Pacheco (2000). For an equatorial ellipticity of $\epsilon$ = 10$^{-6}$, the equivalent density parameter due to gravitational waves has a maximum amplitude in the range 2$\times10^{-11}-3\times10^{-9}$, around 0.9-1.5 kHz. The main reasons affecting the theoretical predictions are discussed. This background is comparable to that produced by the ''ring-down'' emission from distorted black holes. The detection possibility of this background by a future generation of gravitational antennas is also examined.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The extragalactic background of gravitational waves produced by tri-axial rotating neutron stars was calculated, under the assumption that the properties of the underlying pulsar population are the same of those of the galactic population, recently derived by Regimbau & de Freitas Pacheco (2000). | contribution 0.83 | 0.79 | 0.09 | asserted 1.00 |
| s1 | For an equatorial ellipticity of $\epsilon$ = 10$^{-6}$, the equivalent density parameter due to gravitational waves has a maximum amplitude in the range 2$\times10^{-11}-3\times10^{-9}$, around 0.9-1.5 kHz. | result 1.00 | 0.81 | 0.56 | asserted 1.00 |
| s2 | The main reasons affecting the theoretical predictions are discussed. | interpretation 0.46 | 0.53 | 0.03 | unclear 0.63 |
| s3 | This background is comparable to that produced by the ''ring-down'' emission from distorted black holes. | interpretation 0.71 | 0.52 | 0.17 | asserted 1.00 |
| s4 | The detection possibility of this background by a future generation of gravitational antennas is also examined. | contribution 0.60 | 0.74 | 0.07 | unclear 0.46 |
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The paper
Original abstract
The extragalactic background of gravitational waves produced by tri-axial rotating neutron stars was calculated, under the assumption that the properties of the underlying pulsar population are the same of those of the galactic population, recently derived by Regimbau & de Freitas Pacheco (2000). For an equatorial ellipticity of $\epsilon$ = 10$^{-6}$, the equivalent density parameter due to gravitational waves has a maximum amplitude in the range 2$\times10^{-11}-3\times10^{-9}$, around 0.9-1.5 kHz. The main reasons affecting the theoretical predictions are discussed. This background is comparable to that produced by the ''ring-down'' emission from distorted black holes. The detection possibility of this background by a future generation of gravitational antennas is also examined.
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References
How the literature uses it
6 arXiv papers cite this in 7 sentences
Papers citing it · 1 sentence without a confident label
Cites it as background 6 papers
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The possibility of detecting gravitational wave backgrounds generated by an ensemble of neutron stars and of magnetars more specifically, has been discussed by several authors [ref] .
Ultrahigh energy cosmic ray acceleration in newly born magnetars and their associated gravitational wave signatures · Diffuse gravitational wave signals expected for magnetar populations that are sources of the observed UHECR flux · 0.96
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Besides single source signals, the population of rotating neutron stars can contribute to the so-called stochastic GW background (SGWB) [ref] .
Probing the Fermi-LAT GeV excess with gravitational waves · Introduction · 0.96
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A SGWB can be generated by large variety of phenomena of astrophysical (such as CBCs [ref] , isolated neutron stars (NSs) [ref] , NS modes [ref] , core collapses to supernovae [ref] , stellar core collapses to black holes [ref] ) or cosmological (such as cosmic strings [ref] , first order phase transitions [ref] , primordial black holes [ref] , domain walls [ref] , inflation [ref] , pre big bang models [ref] ) origin and hence exist as a superposition of different components.
Estimating Astrophysical Population Properties using a multi-component Stochastic Gravitational-Wave Background Search · Introduction · 0.96
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