Cosmic strings in unified gauge theories

Everett, Allen E.

doi:10.1103/physrevd.24.858

Cited by 149 publications

(113 citation statements)

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“…Such loops are relevant mainly at early times or for small string tensions µ. After a possible early friction-dominated evolution (where the motion of the strings is heavily damped due to their interactions with particles in the high-density thermal plasma [61,62]), a network of cosmic strings enter a scaling regime where its energy density remains a fixed fraction of the total energy density of the universe. The effect of the friction-dominated epoch, in particular for cosmic super-strings, will be discussed in subsection IV B.…”

Section: Consequences For the Loop Number Density And The Frictiomentioning

confidence: 99%

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Cosmic super-strings and Kaluza-Klein modes

Dufaux¹

2012

J. Cosmol. Astropart. Phys.

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Cosmic super-strings interact generically with a tower of relatively light and/or strongly coupled Kaluza-Klein (KK) modes associated with the geometry of the internal space. In this paper, we study the production of spin-2 KK particles by cusps on loops of cosmic F-and D-strings. We consider cosmic super-strings localized either at the bottom of a warped throat or in a flat internal space with large volume. The total energy emitted by cusps in KK modes is comparable in both cases, although the number of produced KK modes may differ significantly. We then show that KK emission is constrained by the photo-dissociation of light elements and by observations of the diffuse gamma ray background. We show that this rules out regions of the parameter space of cosmic super-strings that are complementary to the regions that can be probed by current and upcoming gravitational wave experiments. KK modes are also expected to play an important role in the friction-dominated epoch of cosmic super-string evolution.

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Section: Consequences For the Loop Number Density And The Frictiomentioning

confidence: 99%

“…After their formation at time t f ∼ t Pl /(Gµ), the motion of field theory cosmic strings is usually heavily damped due to their interactions with the high-density thermal plasma of the universe [61,62]. This friction-dominated, or damped evolution ends at the time [1] …”

Section: B Consequences Of the Friction-dominated Epochmentioning

confidence: 99%

Cosmic super-strings and Kaluza-Klein modes

Dufaux¹

2012

J. Cosmol. Astropart. Phys.

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“…Cosmic strings play an important role in the study of the early universe. These strings arise during the phase transition after the big bang explosion as the temperature goes down below some critical temperature as predicted by grand unified theories [1][2][3][4][5]. It is believed that cosmic strings give rise to density perturbations which lead to formation of galaxies [6].…”

Section: Introductionmentioning

confidence: 99%

Cylindrically symmetric inhomogeneous universe with electromagnetic field in string cosmology

Pradhan

Rai

Singh³

2007

Astrophys Space Sci

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Cylindrically symmetric inhomogeneous string cosmological model in presence of electromagnetic field is investigated. We have assumed that F 12 is the only non-vanishing component of F ij . The Maxwell's equations show that F 12 is the function of x alone whereas the magnetic permeability is the function of x and t both. To get the deterministic solution, it has been assumed that the expansion (θ) in the model is proportional to the eigen value 1 1 σ of the shear tensor .i j σ The physical and geometric aspects of the model are also discussed.

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“…The presence of strings in the early universe can be explained using grand unified field theories as investigated by Kibble [1,2], Everett [3] and Vilenkin [4]. It is believed that the very early universe underwent phase transition giving some topological stable structure.…”

Section: Introductionmentioning

confidence: 99%