Stochastic gravitational wave background from smoothed cosmic string loops
By Jose J. Blanco-Pillado, Ken D. Olum. 2017
198 citations recorded by the source corpus.
We do a complete calculation of the stochastic gravitational wave background to be expected from cosmic strings. We start from a population of string loops taken from simulations, smooth these by Lorentzian convolution as a model of gravitational back reaction, calculate the average spectrum of gravitational waves emitted by the string population at any given time, and propagate it through a standard model cosmology to find the stochastic background today. We take into account all known effects, including changes in the number of cosmological relativistic degrees of freedom at early times and the possibility that some energy is in rare bursts that we might never have observed.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/935d8198862c9e71bc527313693793c64ea3108b
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In Astronomy and Astrophysics
- Marek Lewicki
- C. Caprini
- G. Servant
- Daniel G. Figueroa
- P. Simakachorn
- Y. Gouttenoire
- Jose J. Blanco-Pillado
- Marco Peloso
In Nuclear and High Energy Physics
- C. Caprini
- Marek Lewicki
- G. Servant
- Jose J. Blanco-Pillado
- Daniel G. Figueroa
- P. Simakachorn
- Y. Gouttenoire
- Marco Peloso
Citations in the corpus
- The landscape of QCD axion models (2020, background): “Although in principle the length of the loops formed could be ranging at any size, numerical simulations [203, 233–238] show that the initial length of the large loop at its formation tracks the time of formation as”
- Probing the gravitational wave background from cosmic strings with LISA (2019, methodology): “Numerical simulations studying the strings scaling have typically been performed in fixed backgrounds: pure radiation domination and pure matter domination [54, 82, 101, 128].”
- Probing the pre-BBN universe with gravitational waves from cosmic strings (2018, methodology): “ely constant loop size parameter [85{91]. We make the simplifying assumption of monochromatic (large) loop formation with = 0:1, which gives a good reproduction of the loop size distribution of Refs. [90,91]. We comment on the impact of modifying the value of in Section4.3. The formation rate of (la”
- Reconstructing the spectral shape of a stochastic gravitational wave background with LISA (2019, background): “a kination dominated phase [46–50], non-perturbative particle production phenomena [51–62], oscillon dynamics [63–67], strong first order phase transitions [68–81], or cosmic defect networks [82–93].”
- Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies (2020, methodology): “Estimates from simple loops [216–218], as well as results from Nambu-Goto simulations [219], suggest that Γ = 50.”
- New limits on cosmic strings from gravitational wave observation (2017, methodology): “[8], which extracted loops from simulations, smoothed them to model the change of shape due to gravitational back reaction, computed the gravitational power from each loop and propagated the resulting gravitational waves to find the present-day stochastic background.”
- Beyond the Standard Models with cosmic strings (2019, methodology): “nstant, critical density Heaviside function a scale factor of the universe (we solve the full Friedmann equation for a given energy density content); gravitational loop-emission eciency, ( ’50 [149]) (k) Fourier modes of , dependent on the loop small-scale structures, ( (k) /k 4=3 for cusps, e.g”