Effects of biases in domain wall network evolution. II. Quantitative analysis

Correia, J. R. C. C. C.; Leite, Isaura; Martins, C. J. A. P.

doi:10.1103/physrevd.97.083521

Cited by 13 publications

(11 citation statements)

References 20 publications

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“…Specifically, for domain walls the improved VOS model includes separate energy loss terms from both scalar radiation and from chopping of wall blobs (the analogues of cosmic string loops), with the former clearly being the dominant one. In parallel, a General Purpose Graphics Processing Unit (GPU) implementation of the evolution of cosmological domain wall networks has also been developed [24], and its results agree with previous codes [25].…”

Section: Introductionsupporting

confidence: 54%

Extending and calibrating the velocity dependent one-scale model for cosmic strings with one thousand field theory simulations

Correia

Martins

2019

Phys. Rev. D

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Understanding the evolution and cosmological consequences of topological defect networks requires a combination of analytic modeling and numerical simulations. The canonical analytic model for defect network evolution is the Velocity-dependent One-Scale (VOS) model. For the case of cosmic strings, this has so far been calibrated using small numbers of Goto-Nambu and field theory simulations, in the radiation and matter eras, as well as in Minkowski spacetime. But the model is only as good as the available simulations, and it should be extended as further simulations become available. In previous work we presented a General Purpose Graphics Processing Unit implementation of the evolution of cosmological domain wall networks, and used it to obtain an improved VOS model for domain walls. Here we continue this effort, exploiting a more recent analogous code for local Abelian-Higgs string networks. The significant gains in speed afforded by this code enabled us to carry out 1032 field theory simulations of 512 3 size, with 43 different expansion rates. This detailed exploration of the effects of the expansion rate on the network properties in turn enables a statistical separation of various dynamical processes affecting the evolution of the network. We thus extend and accurately calibrate the VOS model for cosmic strings, including separate terms for energy losses due to loop production and scalar/gauge radiation. By comparing this newly calibrated VOS model with the analogous one for domain walls we quantitatively show that energy loss mechanisms are different for the two types of defects.

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Section: Introductionsupporting

confidence: 54%

Extending and calibrating the velocity dependent one-scale model for cosmic strings with one thousand field theory simulations

Correia

Martins

2019

Phys. Rev. D

Self Cite

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“…It was argued in refs. [91][92][93][94][95] that, with a biased initial condition, the domain-wall network follows the scaling solution only for a finite time. In the case of a Z 2 domain-wall model, the domain walls collapse during several Hubble times after the formation unless the probability falling into one of the vacua is very close to 0.5.…”

Section: Discussionmentioning

confidence: 98%

Kilobyte Cosmic Birefringence from ALP domain walls

Takahashi

Yin

2021

J. Cosmol. Astropart. Phys.

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ALP domain walls without strings may be formed in the early Universe. We point out that such ALP domain walls lead to both isotropic and anisotropic birefringence of cosmic microwave background (CMB) polarization, which reflects spatial configuration of the domain walls at the recombination. The polarization plane of the CMB photon coming from each domain is either not rotated at all or rotated by a fixed angle. For domain walls following the scaling solution, the cosmic birefringence of CMB is characterized by 2 N , i.e. N-bit, of information with N = 𝒪(103-4) being equal to the number of domains at the last scattering surface, and thus the name, kilobyte cosmic birefringence. The magnitude of the isotropic birefringence is consistent with the recently reported value, while the anisotropic one is determined by the structure of domains at the last scattering surface. The predicted cosmic birefringence is universal over a wide range of the ALP mass and coupling to photons. The detection of both signals will be a smoking-gun evidence for the ALP domain walls without strings.

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“…We identified relative importance of these factors on fate and decay time of the networks. Effects of part of these factors were studied in the past [3][4][5], however broad analysis was performed for a first time. Moreover, the shaped of the potential around minimum was mentioned as a factor that can influence the stability of the network [3], but this hypothesise was not verified till now.…”

Section: Discussionmentioning

confidence: 99%

“…• infinite domain walls stretching through the whole Universe, depending on the initial contributions of the vacua [1][2][3][4][5]. During further evolution domains are stretched by the expansion of the Universe, thus both the surface and the curvature radius of domain walls grow.…”

Section: Introductionmentioning

confidence: 99%

Stability of domain walls in models with asymmetric potentials

Krajewski,

Kwapisz,

Lalak

et al. 2021

Preprint

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We study the evolution of cosmological domain walls in models with asymmetric potentials. Our research goes beyond the standard case of spontaneous breaking of an approximate symmetry. When the symmetry is explicitly broken the potential exhibits nearly degenerate minima which can lead to creation of a metastable network of domain walls. The time after which the network will decay depends on the difference of values of the potential in minima, its asymmetry around the maximum separating minima and the bias of initial distribution. Using numerical lattice simulations we determine relative importance of these factors on decay time of networks for generic potentials. We find that even very small departures from the symmetric case lead to rapid decay of the domain wall network. As a result creation of a long lasting network capable of producing observable gravitational wave signals is much more difficult than previously thought.

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Effects of biases in domain wall network evolution. II. Quantitative analysis

Cited by 13 publications

References 20 publications

Extending and calibrating the velocity dependent one-scale model for cosmic strings with one thousand field theory simulations

Extending and calibrating the velocity dependent one-scale model for cosmic strings with one thousand field theory simulations

Kilobyte Cosmic Birefringence from ALP domain walls

Stability of domain walls in models with asymmetric potentials

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