Topology of cosmic domains and strings

Kibble, T. W. B.

doi:10.1088/0305-4470/9/8/029

Cited by 4,413 publications

(4,981 citation statements)

References 13 publications

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“…(1) is σ 2 S D with S D = 2π D/2 /Γ(D/2) being the total area of the surface of the unit sphere in D-dimensional Euclidean space. This leads to the solid angle deficit (1 − σ 2 )S D in the spacetime given by line element (1). It is of interest to note that the effective metric produced in superfluid 3 He − A by a monopole is described by the three dimensional version of the line element (1) with the negative angle deficit, σ > 1, which corresponds to the negative mass of the topological object [19].…”

Section: Wightman Functionmentioning

confidence: 99%

“…With this coordinate, in general, we will obtain non-standard angular part in the exterior line element (1). For the metric corresponding to line element (2) the nonzero components of the Ricci tensor are given by expressions (no summation over i, we adopt the convention of Birrell and Davies [20] for the curvature tensor)…”

Section: Wightman Functionmentioning

confidence: 99%

“…It is well known that different types of topological objects may have been formed in the early universe after Planck time by the vacuum phase transition [1,2]. Depending on the topology of the vacuum manifold these are domain walls, strings, monopoles and textures.…”

Section: Introductionmentioning

confidence: 99%

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Vacuum polarization by a global monopole with finite core

Mello

Saharian

2006

J. High Energy Phys.

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We investigate the effects of a (D + 1)-dimensional global monopole core on the behavior of a quantum massive scalar field with general curvature coupling parameter. In the general case of the spherically symmetric static core, formulae are derived for the Wightman function, for the vacuum expectation values of the field square and the energy-momentum tensor in the exterior region. These expectation values are presented as the sum of point-like global monopole part and the core induced one. The asymptotic behavior of the core induced vacuum densities is investigated at large distances from the core, near the core and for small values of the solid angle corresponding to strong gravitational fields. In particular, in the latter case we show that the behavior of the vacuum densities is drastically different for minimally and non-minimally coupled fields. As an application of general results the flowerpot model for the monopole's core is considered and the expectation values inside the core are evaluated.

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Section: Wightman Functionmentioning

confidence: 99%

Section: Wightman Functionmentioning

confidence: 99%

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Vacuum polarization by a global monopole with finite core

Mello

Saharian

2006

J. High Energy Phys.

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“…Since the Planck time, the Universe has, through its expansion, steadily cooled down and a series of phase transitions followed by Spontaneously Symmetry Breaking 2 (SSBs) took place in the framework of GUTs. Such SSBs may have left behind topological defects as false vacuum remnants, via the Kibble mechanism [6].…”

Section: Topological Defects In Gutsmentioning

confidence: 99%

Cosmic Strings and Cosmic Superstrings

Sakellariadou

2009

Nuclear Physics B - Proceedings Supplements

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In these lectures, I review the current status of cosmic strings and cosmic superstrings. I first discuss topological defects in the context of Grand Unified Theories, focusing in particular in cosmic strings arising as gauge theory solitons. I discuss the reconciliation between cosmic strings and cosmological inflation, I review cosmic string dynamics, cosmic string thermodynamics and cosmic string gravity, which leads to a number of interesting observational signatures. I then proceed with the notion of cosmic superstrings arising at the end of brane inflation, within the context of brane-world cosmological models inspired from string theory. I discuss the differences between cosmic superstrings and their solitonic analogues, I review our current understanding about the evolution of cosmic superstring networks, and I then briefly describe the variety of observational consequences, which may help us to get an insight into the stringy description of our Universe.

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“…Domain walls form when a discrete symmetry is spontaneously broken [1][2][3][4][5]. In simplest models, symmetry breaking is accomplished by a real scalar field φ whose vacuum manifold is disconnected.…”

Section: Introductionmentioning

confidence: 99%

Plane symmetric bulk viscous domain wall in Lyra geometry

Pradhan

Kumar

Yadav³

2007

Braz. J. Phys.

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In this paper general solutions are found for domain walls in Lyra geometry in the plane symmetric spacetime metric given by Taub. Expressions for the energy density and pressure of domain walls are derived in both cases of uniform and time varying displacement field β. Some physical consequences of the models are also given. Finally, the geodesic equations and acceleration of the test particle are discussed.

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Topology of cosmic domains and strings

Cited by 4,413 publications

References 13 publications

Vacuum polarization by a global monopole with finite core

Vacuum polarization by a global monopole with finite core

Cosmic Strings and Cosmic Superstrings

Plane symmetric bulk viscous domain wall in Lyra geometry

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