84 research outputs found
The bispectrum of matter perturbations from cosmic strings
We present the first calculation of the bispectrum of the matter perturbations induced by cosmic strings. The calculation is performed in two different ways: the first uses the unequal time correlators (UETCs) of the string network - computed using a Gaussian model previously employed for cosmic string power spectra. The second approach uses the wake model, where string density perturbations are concentrated in sheet-like structures whose surface density grows with time. The qualitative and quantitative agreement of the two gives confidence to the results. An essential ingredient in the UETC approach is the inclusion of compensation factors in the integration with the Green's function of the matter and radiation fluids, and we show that these compensation factors must be included in the wake model also. We also present a comparison of the UETCs computed in the Gaussian model, and those computed in the unconnected segment model (USM) used by the standard cosmic string perturbation package CMBACT. We compare numerical estimates for the bispectrum of cosmic strings to those produced by perturbations from an inflationary era, and discover that, despite the intrinsically non-Gaussian nature of string-induced perturbations, the matter bispectrum is unlikely to produce competitive constraints on a population of cosmic strings
Scaling in a SU(2)/Z_3 model of cosmic superstring networks
Motivated by recent developments in superstring theory in the cosmological
context, we examine a field theory which contains string networks with 3-way
junctions. We perform numerical simulations of this model, identify the length
scales of the network that forms, and provide evidence that the length scales
tend towards a scaling regime, growing in proportion to time. We infer that the
presence of junctions does not in itself cause a superstring network to
dominate the energy density of the early Universe.Comment: 12pp, 3 fig
Defect Production in Slow First Order Phase Transitions
We study the formation of vortices in a U(1) gauge theory following a
first-order transition proceeding by bubble nucleation, in particular the
effect of a low velocity of expansion of the bubble walls. To do this, we use a
two-dimensional model in which bubbles are nucleated at random points in a
plane and at random times and then expand at some velocity .
Within each bubble, the phase angle is assigned one of three discrete values.
When bubbles collide, magnetic `fluxons' appear: if the phases are different, a
fluxon--anti-fluxon pair is formed. These fluxons are eventually trapped in
three-bubble collisions when they may annihilate or form quantized vortices. We
study in particular the effect of changing the bubble expansion speed on the
vortex density and the extent of vortex--anti-vortex correlation.Comment: 13 pages, RevTeX, 15 uuencoded postscript figure
Scaling in Numerical Simulations of Domain Walls
We study the evolution of domain wall networks appearing after phase
transitions in the early Universe. They exhibit interesting dynamical scaling
behaviour which is not yet well understood, and are also simple models for the
more phenomenologically acceptable string networks. We have run numerical
simulations in two- and three-dimensional lattices of sizes up to 4096^3. The
theoretically predicted scaling solution for the wall area density A ~ 1/t is
supported by the simulation results, while no evidence of a logarithmic
correction reported in previous studies could be found. The energy loss
mechanism appears to be direct radiation, rather than the formation and
collapse of closed loops or spheres. We discuss the implications for the
evolution of string networks.Comment: 7pp RevTeX, 9 eps files (including six 220kB ones
Gravitational Radiation by Cosmic Strings in a Junction
The formalism for computing the gravitational power radiation from
excitations on cosmic strings forming a junction is presented and applied to
the simple case of co-planar strings at a junction when the excitations are
generated along one string leg. The effects of polarization of the excitations
and of the back-reaction of the gravitational radiation on the small scale
structure of the strings are studied.Comment: minor changes added, the published version in JCA
Estimation of vortex density after superconducting film quench
This paper addresses the problem of vortex formation during a rapid quench in
a superconducting film. It builds on previous work showing that in a local
gauge theory there are two distinct mechanisms of defect formation, based on
fluctuations of the scalar and gauge fields, respectively. We show how vortex
formation in a thin film differs from the fully two-dimensional case, on which
most theoretical studies have focused. We discuss ways of testing theoretical
predictions in superconductor experiments and analyse the results of recent
experiments in this light.Comment: 7 pages, no figure
The effects of inhomogeneities on the cosmology of type IIB conifold transitions
In this paper we examine the evolution of the effective field theory
describing a conifold transition in type IIB string theory. Previous studies
have considered such dynamics starting from the cosmological approximation of
homogeneous fields, here we include the effects of inhomogeneities by using a
real-time lattice field theory simulation. By including spatial variations we
are able to simulate the effect of currents and the gauge fields which they
source. We identify two different regimes where the inhomogeneities have
opposite effects, one where they aid the system to complete the conifold
transition and another where they hinder it. The existence of quantized fluxes
in related systems has lead to the speculation that (unstable) string solutions
could exist, using our simulations we give strong evidence that these
string-like defects do not form.Comment: 11 pages, 2 figures. Published versio
Universality and Critical Phenomena in String Defect Statistics
The idea of biased symmetries to avoid or alleviate cosmological problems
caused by the appearance of some topological defects is familiar in the context
of domain walls, where the defect statistics lend themselves naturally to a
percolation theory description, and for cosmic strings, where the proportion of
infinite strings can be varied or disappear entirely depending on the bias in
the symmetry. In this paper we measure the initial configurational statistics
of a network of string defects after a symmetry-breaking phase transition with
initial bias in the symmetry of the ground state. Using an improved algorithm,
which is useful for a more general class of self-interacting walks on an
infinite lattice, we extend the work in \cite{MHKS} to better statistics and a
different ground state manifold, namely , and explore various different
discretisations. Within the statistical errors, the critical exponents of the
Hagedorn transition are found to be quite possibly universal and identical to
the critical exponents of three-dimensional bond or site percolation. This
improves our understanding of the percolation theory description of defect
statistics after a biased phase transition, as proposed in \cite{MHKS}. We also
find strong evidence that the existence of infinite strings in the Vachaspati
Vilenkin algorithm is generic to all (string-bearing) vacuum manifolds, all
discretisations thereof, and all regular three-dimensional lattices.Comment: 62 pages, plain LaTeX, macro mathsymb.sty included, figures included.
also available on
http://starsky.pcss.maps.susx.ac.uk/groups/pt/preprints/96/96011.ps.g
Characteristic length scales and formation of vortices in the Abelian Higgs model in the presence of a uniform background charge
In this brief report we consider a non-local Abelian Higgs model in the
presence of a neutralizing uniform background charge. We show that such a
system possesses vortices which key feature is a strong radial electric field.
We estimate the basic properties of such an object and characteristic length
scales in this model.Comment: Replaced with journal version. Some minor change
Fermionic Zero Modes of Supergravity Cosmic Strings
Recent developments in string theory suggest that cosmic strings could be
formed at the end of brane inflation. Supergravity provides a realistic model
to study the properties of strings arising in brane inflation. Whilst the
properties of cosmic strings in flat space-time have been extensively studied
there are significant complications in the presence of gravity. We study the
effects of gravitation on cosmic strings arising in supergravity. Fermion zero
modes are a common feature of cosmic strings, and generically occur in
supersymmetric models. The corresponding massless currents can give rise to
stable string loops (vortons). The vorton density in our universe is strongly
constrained, allowing many theories with cosmic strings to be ruled out. We
investigate the existence of fermion zero modes on cosmic strings in
supergravity theories. A general index theorem for the number of zero modes is
derived. We show that by including the gravitino, some (but not all) zero modes
disappear. This weakens the constraints on cosmic string models. In particular,
winding number one cosmic D-strings in models of brane inflation are not
subject to vorton constraints. We also discuss the effects of supersymmetry
breaking on cosmic D-strings.Comment: 33 page
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