Transitions between topologically non-trivial configurations

Gani, Vakhid A.; Кириллов, А. А.; Rubin, S. G.

doi:10.1088/1742-6596/934/1/012046

Cited by 15 publications

(13 citation statements)

References 49 publications

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“…Furthermore, we set R = ϕ 2 0 + χ 2 0 , see figure 1 (right panel). We performed the numerical simulation of the evolution of the initial configuration (4.2), (4.3) for N = 1, 2, 3, 4 and confirmed possibility of soliton production for all N , which was shown earlier in [64]. Our results are presented in figures 2 and 3.…”

Section: The Winding Numbersupporting

confidence: 80%

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Classical transitions with the topological number changing in the early Universe

Gani

Кириллов

Rubin

2018

J. Cosmol. Astropart. Phys.

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We consider classical dynamics of two real scalar fields within a model with the potential having a saddle point. The solitons of such model are field configurations that have the form of closed loops in the field space. We study the formation and evolution of these solitons, in particular, the conditions at which they could be formed even when the model potential has only one minimum. These non-trivial field configurations represent domain walls in the three-dimensional physical space. The set of these configurations can be split into disjoint equivalence classes. We provide a simple expression for the winding number of an arbitrary closed loop in the field space and discuss the transitions that change the winding number. We also show that non-trivial field configurations could be responsible for the energy density excess that could evade the CMB constraints but could be important at scales which are responsible for the formation of galaxies and the massive primordial black holes.

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Section: The Winding Numbersupporting

confidence: 80%

“…For N > 2 the number of "humps" is increasing proportional to N (see [64] for details). If the height of the potential maximum is small enough, the fields overcome the maximum and tend to the absolute minimum in the whole space.…”

Section: The Winding Numbermentioning

confidence: 99%

Classical transitions with the topological number changing in the early Universe

Gani

Кириллов

Rubin

2018

J. Cosmol. Astropart. Phys.

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“…[88][89][90][91][92][93]. Topologically non-trivial field configurations could be responsible for a variety of phenomena observed in the early Universe [94,95].…”

Section: Introductionmentioning

confidence: 99%

Scattering of the φ8 kinks with power-law asymptotics

Belendryasova

Gani

2019

Communications in Nonlinear Science and Numerical Simulation

104

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We study the scattering of the ϕ 8 kinks off each other, namely, we consider those ϕ 8 kinks that have power-law asymptotics. The slow power-law fall-off leads to a long-range interaction between the kink and the antikink. We investigate how the scattering scenarios depend on the initial velocities of the colliding kinks. In particular, we observe the 'escape windows' -the escape of the kinks after two or more collisions, explained by the resonant energy exchange between the translational and vibrational modes. In order to elucidate this phenomenon, we also analyze the excitation spectra of a solitary kink and of a composite kink+antikink configuration.

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“…5 The mechanism of the wall formation is quite general and can be applied to those inflationary models containing extrema of their potential. Some of them where developed in [35][36][37] and in [38,39] where the potentials with saddle points were considered. It has been revealed there that the PBH mass spectrum and PBH ability depend strongly on the potential parameters and an initial field value, see discussion in Section 4 1.…”

Section: Introductionmentioning

confidence: 99%

Clusters of Primordial Black Holes

et al. 2019

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The Primordial Black Holes (PBHs) are a well-established probe for new physics in the very early Universe. We discuss here the possibility of PBH agglomeration into clusters that may have several prominent observable features. The clusters can form due to closed domain walls appearance in the natural and hybrid inflation models whose subsequent evolution leads to PBH formation. The dynamical evolution of such clusters discussed here is of crucial importance. Such a model inherits all the advantages of uniformly distributed PBHs, like possible explanation of supermassive black holes existence (origin of the early quasars), the binary black hole mergers registered by LIGO/Virgo through gravitational waves, which could provide ways to test the model in future, the contribution to reionization of the Universe. If PBHs form clusters, they could alleviate or completely avoid existing constraints on the abundance of uniformly distributed PBHs, thus allowing PBH to be a viable dark matter candidate. Most of the existing constraints on uniform PBH density should be re-considered to the case of PBH clustering. Furthermore, unidentified cosmic gamma-ray point-like sources could be (partially) accounted. We conclude that models leading to PBH clustering are favored compared to models predicting the uniform distribution of PBHs.

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Transitions between topologically non-trivial configurations

Cited by 15 publications

References 49 publications

Classical transitions with the topological number changing in the early Universe

Classical transitions with the topological number changing in the early Universe

Scattering of the φ8 kinks with power-law asymptotics

Clusters of Primordial Black Holes

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