Ionization from cosmic strings at cosmic dawn

Laliberte, Samuel; Brandenberger, Robert H.

doi:10.1103/physrevd.101.023528

Cited by 6 publications

(4 citation statements)

References 57 publications

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“…This is the value of Gµ when particle production is as efficient as gravitational production. For example for loops created at the recombination time, the value of Gµ maximizing the cosmic ray production is 10 −18 [272].…”

Section: Jcap07(2020)032mentioning

confidence: 99%

“…Also, electromagnetic radiation, by increasing the ionization fraction of neutral hydrogen, can affect the CMB temperature and polarization correlation functions at large angular scales, leading to the contraint I 10 7 GeV [292]. Note that ionization of neutral hydrogen has been studied in [272] in the case of non-superconducting strings. Additionally, the radio emission from SCS can increase the depth of the 21 cm absorption signal, and EDGES data excludes the SCS tension Gµ ∼ 10 −13 for string currents as low at I ∼ 10 GeV.…”

Section: Jcap07(2020)032mentioning

confidence: 99%

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Beyond the Standard Models with cosmic strings

Gouttenoire

Servant

Simakachorn

2020

J. Cosmol. Astropart. Phys.

144

204

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We examine which information on the early cosmological history can be extracted from the potential measurement by third-generation gravitational-wave observatories of a stochastic gravitational wave background (SGWB) produced by cosmic strings. We consider a variety of cosmological scenarios breaking the scale-invariant properties of the spectrum, such as early long matter or kination eras, short intermediate matter and inflation periods inside a radiation era, and their specific signatures on the SGWB. This requires to go beyond the usually-assumed scaling regime, to take into account the transient effects during the change of equation of state of the universe. We compute the time evolution of the string network parameters and thus the loop-production efficiency during the transient regime, and derive the corresponding shift in the turning-point frequency. We consider the impact of particle production on the gravitational-wave emission by loops. We estimate the reach of future interferometers LISA, BBO, DECIGO, ET and CE and radio telescope SKA to probe the new physics energy scale at which the universe has experienced changes in its expansion history. We find that a given interferometer may be sensitive to very different energy scales, depending on the nature and duration of the non-standard era, and the value of the string tension. It is fascinating that by exploiting the data from different GW observatories associated with distinct frequency bands, we may be able to reconstruct the full spectrum and therefore extract the values of fundamental physics parameters.

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Section: Jcap07(2020)032mentioning

confidence: 99%

Section: Jcap07(2020)032mentioning

confidence: 99%

Beyond the Standard Models with cosmic strings

Gouttenoire

Servant

Simakachorn

2020

J. Cosmol. Astropart. Phys.

144

204

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show abstract

“…The photon flux from unwinding textures can effect more cosmological observables. For example, the extra photon radiation at radio wavelengths may lead to an absorption feature [35] in the global 21cm signal, in the same way that decaying cosmic string loops may yield such a signal [36][37][38]. It is unlikely, however, that unwinding events can explain the origins of fast radio bursts (FRBs), as the decay pattern to low energy photons suffers from similar problems to those photons produced off of cosmic string cusps [39].…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Cosmic rays and spectral distortions from collapsing textures

Brandenberger

Cyr

Jiao

2020

J. Cosmol. Astropart. Phys.

Self Cite

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We compute the energy spectrum of photons {and neutrinos} produced by the unwinding of a scaling distribution of cosmic textures, and discuss the implications for the spectrum of high energy cosmic rays, and for CMB spectral distortions. Textures lead to a contribution to the photon flux which scales as E3 F(E) ∼ E3/2. Hence, the tightest constraints on the texture model come from the highest energies from which primordial photons can reach us without being scattered by the CMB and other foregrounds. Textures lead to both μ type and y type distortions. While the constraints on the texture model coming from the current COBE bounds are weaker than the bounds from the angular power spectrum of the CMB, future surveys such as PIXIE can lead to stronger bounds. {The high energy neutrino flux is constrained by data from the Pierre Auger experiment and yields a bound on the energy scale of textures which is competitive with CMB bounds.}

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“…There are also Gµ measurements and forecasts from other observational routes. For example see Ringeval & Suyama (2017) Kuroyanagi et al (2013) for bounds on string loops from pulsar timing constraints on the amplitude of the stochastic gravitational wave background, Imtiaz et al (2020) for bounds on CS network from fast radio bursts, Brandenberger et al (2010); Hernandez & Brandenberger (2012); Pagano & Brandenberger (2012) for forecasts from 21-cm signatures, Laliberte & Brandenberger (2020) for CS imprints on ionization fraction in the Universe, Fernandez et al (2020) for the effect of CS on the filament structure in the cosmic web and Cunha et al (2018) for the imprint of CSs on the dark matter distribution.…”

Section: )mentioning

confidence: 99%

Planck Limits on Cosmic String Tension Using Machine Learning

Torki,

Hajizadeh,

Farhang

et al. 2021

Preprint

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We develop two parallel machine-learning pipelines to estimate the contribution of cosmic strings (CSs), conveniently encoded in their tension (Gµ), to the anisotropies of the cosmic microwave background radiation observed by Planck. The first approach is tree-based and feeds on certain map features derived by image processing and statistical tools. The second uses convolutional neural network with the goal to explore possible non-trivial features of the CS imprints. The two pipelines are trained on Planck simulations and when applied to Planck SMICA map yield the 3σ upper bound of Gµ 8.6 × 10 −7 . We also train and apply the pipelines to make forecasts for futuristic CMB-S4-like surveys and conservatively find their minimum detectable tension to be Gµ min ∼ 1.9 × 10 −7 .

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Ionization from cosmic strings at cosmic dawn

Cited by 6 publications

References 57 publications

Beyond the Standard Models with cosmic strings

Beyond the Standard Models with cosmic strings

Cosmic rays and spectral distortions from collapsing textures

Planck Limits on Cosmic String Tension Using Machine Learning

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