Magnetic Field of Cosmic Strings in the Early Universe

Zadorozhna, L.V.; Hnatyk, B.; Sitenko, Yu. A.

doi:10.15407/ujpe58.04.0398

Cited by 6 publications

(6 citation statements)

References 9 publications

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“…These fields would be among the distinctive features of the cosmic strings produced during the inflation and also of the corresponding inflationary models. Note that various types of mechanisms for the generation of primordial magnetic fields from cosmic strings in the postinflationary era have been discussed in the literature (see, for instance, [56][57][58][59][60][61][62][63]). For cosmic strings carrying a nonzero magnetic flux in the core, azimuthal currents for charged fields are generated around the string (see [30,31] and the references therein).…”

Section: Magnetic Field Correlators and Vev Of The Energy Densitymentioning

confidence: 99%

Electromagnetic vacuum fluctuations around a cosmic string in de Sitter spacetime

2017

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The electromagnetic field correlators are evaluated around a cosmic string in background of (D + 1)-dimensional dS spacetime assuming that the field is prepared in the Bunch-Davies vacuum state. The correlators are presented in the decomposed form where the string-induced topological parts are explicitly extracted. With this decomposition, the renormalization of the local vacuum expectation values (VEVs) in the coincidence limit is reduced to the one for dS spacetime in the absence of the cosmic string. The VEVs of the squared electric and magnetic fields, and of the vacuum energy density are investigated. Near the string they are dominated by the topological contributions and the effects induced by the background gravitational field are small. In this region, the leading terms in the topological contributions are obtained from the corresponding VEVs for a string on the Minkowski bulk multiplying by the conformal factor. At distances from the string larger than the curvature radius of the background geometry, the pure dS parts in the VEVs dominate. In this region, for spatial dimensions D > 3, the influence of the gravitational field on the topological contributions is crucial and the corresponding behavior is essentially different from that for a cosmic string on the Minkowski bulk. There are well-motivated inflationary models which produce cosmic strings. We argue that, as a consequence of the quantum-to-classical transition of super-Hubble electromagnetic fluctuations during inflation, in the post-inflationary era these strings will be surrounded by large-scale stochastic magnetic fields. These fields could be among the distinctive features of the cosmic strings produced during the inflation and also of the corresponding inflationary models.

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Section: Magnetic Field Correlators and Vev Of The Energy Densitymentioning

confidence: 99%

Electromagnetic vacuum fluctuations around a cosmic string in de Sitter spacetime

2017

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“…As a result, they will emit electromagnetic waves in a wide range of energies. In works [11,12], the generation of non-thermal radiation at the interaction between a superconducting string and the cosmic plasma was described in detail.…”

Section: Magnetic Field Around a Gut-stringmentioning

confidence: 99%

Magnetic Field of Cosmic Strings in the Early Universe

Zadorozhna¹,

Hnatyk²,

Sitenko³

2013

Preprint

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Cosmic strings are topological defects which can be formed as a result of phase transitions with a spontaneous symmetry breaking in the early Universe. The possibility of the generation of a magnetic field around a cosmic string on the Grand Unification energy scale (GUT scale) in the early Universe immediately after the termination of the deconfinement-confinement phase transition has been analyzed. It is found that a circular current and a magnetic field directed along the string are induced around the string in the vacuum of a pseudoscalar matter consisting of charged pions. We also have studied the interaction between the magnetic flux tube surrounding the string (the string magnetosphere) and the cosmic plasma in the early Universe. A possibility of magnetization of the cosmic plasma surrounding the string owing to its interaction with the string magnetic field has been analyzed. K e y w o r d s: cosmic string, phase transitions, vacuum polarization effect, ultrarelativistic plasma, vacuum of pseudoscalar matter consisting of charged pions, bow shock, magnetic tube.

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“…There is a phase transition in the cooling time, related to the breaking of the symmetry, that causes topological defects. It is assumed that inflation is driven by the scalar field, namely the inflaton [19]. Moreover, typical dilaton fields are also quite suitable for producing the correct value of the slow-roll of the inflation.…”

Section: Introductionmentioning

confidence: 99%

Light deflection by charged wormholes in Einstein-Maxwell-dilaton theory

2017

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In this paper, we study the deflection of light by a class of charged wormholes within the context of the Einstein-Maxwell-dilaton theory. The primordial wormholes are predicted to exist in the early universe, where inflation driven by the dilaton field. We perform our analysis through optical geometry using the Gibbons-Werner method (GW), by adopting the Gauss-Bonnet theorem and the standard geodesics approach. We report an interesting result for the deflection angle in leadingorder terms-namely, the deflection angle increases due to the electric charge Q and the magnetic charge P , whereas it decreases due to the dilaton charge Σ. Finally, we confirm our findings by means of geodesics equations. Our computations show that the GW method gives an exact result in leading order terms.PACS numbers: 95.30.Sf, 98.62.Sb

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Magnetic Field of Cosmic Strings in the Early Universe

Cited by 6 publications

References 9 publications

Electromagnetic vacuum fluctuations around a cosmic string in de Sitter spacetime

Electromagnetic vacuum fluctuations around a cosmic string in de Sitter spacetime

Magnetic Field of Cosmic Strings in the Early Universe

Light deflection by charged wormholes in Einstein-Maxwell-dilaton theory

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