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2 edition of Complete model and properties of a self-gravitatng cosmic string and of the conical spacetime. found in the catalog.

Complete model and properties of a self-gravitatng cosmic string and of the conical spacetime.

Francine R. Marleau

Complete model and properties of a self-gravitatng cosmic string and of the conical spacetime.

by Francine R. Marleau

  • 166 Want to read
  • 11 Currently reading

Published .
Written in English


The Physical Object
Pagination109 leaves.
Number of Pages109
ID Numbers
Open LibraryOL19511606M
ISBN 100612073459

Self-Gravitating Media Luigi Pilo invariance is unbroken and basically the medium is not present; in the broken phase the fields acquire a vacuum expectation value that is not invariant under spacetime translations. The leading order action in a derivative expansion of a self-gravitating medium in the presence of dynamical gravity, is given by. CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): The kinetic theory of a self-gravitating system is considered in the Bhatnager-Gross-Krook approximation to the kinetic equation. This approach offers a unique and tractable setup for studying the central, collision-dominated region of the system, as well as its almost collisionless outer part.

(There is a conical singularity on the string, yes, but no propagating curvature.) This is where I would really like some elaboration, because it seems intuitive. But I know that the gravitational effect of a slow rolling scalar is counter-intuitive so I don't want to jump to conclusions here. Cosmic strings are very long, thin structures which might stretch over vast reaches of the universe. If they exist, they would have been formed during phase transitions in the very early universe. The space-time surrounding a straight cosmic string is flat but nontrivial: A two-dimensional spatial section is a cone rather than a plane.

2 Cosmic string loop radiation spectrum The spectrum of gravitational radiation emitted by a network of cosmic string loops is obtained using a background Ω = 1 FRW cosmological model, an extended one-scale model for the evolution of a network of cosmic strings, and a model of the emission of gravitational radiation by cosmic string loops. The. It is believed that this theory is an ultra-violet (UV) completion for the classical theory of gravitation. In this paper, after a brief review of some fundamental features of this theory, we investigate it for a static cylindrical symmetric solution which describes \emph{Cosmic string} as .


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Complete model and properties of a self-gravitatng cosmic string and of the conical spacetime by Francine R. Marleau Download PDF EPUB FB2

Gotoaction and secondly the self-gravitating one in which the straight cosmic string in particular is considered as the source of a gravitational field. In this case one finds that the asymptotical metric generated by the straight cosmic string is a conical metric [1] and the case of a singular line is obtained in a limit process.

with the spherical symmetric case and the well known abelian cosmic string solution [12–15], particularly the supermassive case. In these U(1)-gauge cosmic string models it was found that as the energy scale of symmetry breaking increases, the geometry around the string changes from conical to an analog of a Kasner spacetime.

Complete Model of a Self-gravitating Cosmic String I. A New Class of Exact Solutions and Gravitational Lensing Article (PDF Available) in Physical review D: Particles and fields 52(10).

It is well known that static straight local cosmic strings coupled to gravity produce a spacetime with conical sections transverse to the axis of the string. Model of a Self-gravitating Cosmic.

The conical singularity in flat spacetime is mostly known as a model of the cosmic string or the wedge disclination in solids. Another, equally important, function is to be a representative of.

at spacetime with a conical singularity along the world-sheet of the string. The geometry of such a spacetime is completely xed by the holonomy of a simple loop wrapping the conical singularity. In the case of a mass-less cosmic string, this holonomy is a. The coupled Einstein-Yang-Mills equations on a time dependent axially symmetric spacetime are investigated, without a priori any conditions on the gauge field.

There is numerical evidence for the existence of a regular solution with the desired asymptotic features. Just as in the supermassive abelian counterpart model, the formation of a singularity at finite distance of the core of the string.

With the development of the technology of weak lensing, the weak lensing effect produced by a cosmic string could also be a useful tool to constrain the properties of a cosmic string. thin cosmic string and give the complete s et of analytical solutions of this equation for massive and massless particles in terms of Mino time that allows to decouple the r - and θ -component of the.

We assume that a self-gravitating string is locally described by a thin tube of matter represented by a ``smoothed conical metric''. If we impose a specific constraint on the model of string then its central line obeys the Nambu-Goto dynamics in the limit where the radius of the tube tends to zero.

If no constraint is added then the world sheet of the central line is. We examine the coupled Einstem-Euler-Lagrange equations for nonstationary cosmic strings. Self-consistent solutions to all the equations are found under the assumption that the energy-momentum tensor is of the formT t t =T z z while all other components vanish.

It is shown that the strings are necessarily static in this case and that the scalar field potential must be of the usual. CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): The classical Einstein–Maxwell field equations admit static horizonless wormhole solutions with only a circular cosmic string singularity.

We show how to extend these static solutions to exact rotating asymptotically flat solutions. For a suitable range of parameter values, these solutions.

Motivated by the study of self gravitating cosmic strings, we pursue the well known method by C. Bandle to obtain a weak version of the classical Alexandrov's isoperimetric inequality. In fact we derive some quantitative estimates for weak.

CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): Cosmic strings are considered in two types of gauged sigma models, which generalize the gravitating Abelian Higgs model.

The two models differ by whether the U(1) kinetic term is of the Maxwell or Chern-Simons form. We obtain the self-duality conditions for a general two-dimensional target space. We present a family of classical spacetimes in 2+1 dimensions. Such a spacetime is produced by a Nambu-Goto self-gravitating string.

Due to the special. The resulting figures all depend on the particular theory that's employed, but a good rule of thumb is that 1 inch ( centimeters) of cosmic string has about the same mass as Mount Everest, and.

We study field theoretical models for cosmic strings with flat directions in curved space-time. More precisely, we consider minimal models with semilocal, axionic and tachyonic strings, respectively.

In flat space-time, isolated static and straight cosmic strings solutions of these models have a flat direction, i.e., a uniparametric family of configurations with the same. We complete our study of the self-gravitating gas by computing the fluctuations around the saddle point solution for the three statistical ensembles (grand canonical, canonical and microcanonical).

Although the saddle point is the same for the three ensembles, the fluctuations change from one ensemble to the other. Abstract. In the framework of general relativity, an exact axisymmetric (vortex) solution of the equations of motion is obtained for the SU(2) symmetric sigma solution is characterized by the topological charge (winding number) and angular deficit.

Self-gravitating cosmic rings. By G Clément. The classical Einstein--Maxwell field equations admit static horizonless wormhole solutions with only a circular cosmic string singularity. We show how to extend these static solutions to exact rotating asymptotically flat solutions.

For a suitable range of parameter values, these solutions. We provide a complete picture of the self-gravitating non-relativistic gas at thermal equilibrium using Monte Carlo simulations (MC), analytic mean field methods (MF) and low density expansions.

The system is shown to possess an infinite volume limit, both in the canonical (CE) and in the microcanonical ensemble (MCE) when N, V → ∞, keeping.If cosmic strings are measurable which is a real possibility for a wide range of cosmological string models this would provide the first experimental evidence of a string theory model underlying the structure of spacetime.

A string is a geometrical deviation from Euclidean geometry in spacetime characterized by an angular deficit: a circle.The problem of a self-gravitating scalar field with positive cosmological constant Jo˜ao L.

Costa(1,3), Artur Alho(2) and Jos´e Natario(3) (1)Instituto Universitario de Lisboa (ISCTE-IUL), Lisboa, Portugal (2)Centro de Matema´tica, Universidade do Minho, Gualtar, Braga, Portugal (3)Centro de Ana´lise Matema´tica, Geometria e Sistemas Dinˆamicos.