187 research outputs found
Anyonic Bogomol'nyi Solitons in a Gauged O(3) Sigma Model
We introduce the self-dual abelian gauged sigma models where the
Maxwell and Chern-Simons terms constitute the kinetic terms for the gauge
field. These models have quite rich structures and various limits. Our models
are found to exhibit both symmetric and broken phases of the gauge group. We
discuss the pure Chern-Simons limit in some detail and study rotationally
symmetric solitons.Comment: 14 pages, 6 Postscript figures uuencoded, written in REVTe
Bogomolnyi Bound with a Cosmological Constant
Bogomolnyi-type bound is constructed for the topological solitons in O(3)
nonlinear model coupled to gravity with a negative cosmological
constant. Spacetimes made by self-dual solutions form a class of G\"{o}del-type
universe. In the limit of a spinless massive point particle, the obtained
stationary metric does not violate the causality and it is a new point particle
solution different from the known static hyperboloid and black hole. We also
showed that static Nielsen-Olesen vortices saturate Bogomolnyi-type bound only
when the cosmological constant vanishes.Comment: 11 pages, RevTe
Solitons in 1+1 Dimensional Gauged Sigma Models
We study soliton solutions in 1+1 dimensional gauged sigma models, obtained
by dimensional reduction from its 2+1 dimensional counterparts. We show that
the Bogomol'nyi bound of these models can be expressed in terms of two
conserved charges in a similar way to that of the BPS dyons in 3+1 dimensions.
Purely magnetic vortices of the 2+1 dimensional completely gauged sigma model
appear as charged solitons in the corresponding 1+1 dimensional theory. The
scale invariance of these solitons is also broken because of the dimensional
reduction. We obtain exact static soliton solutions of these models saturating
the Bogomol'nyi bound.Comment: 21 pages, RevTeX, minor changes, version to appear in Physical Review
Global Vortex and Black Cosmic String
We study global vortices coupled to (2+1) dimensional gravity with negative
cosmological constant. We found nonsingular vortex solutions in -theory
with a broken U(1) symmetry, of which the spacetimes do not involve physical
curvature singularity. When the magnitude of negative cosmological constant is
larger than a critical value at a given symmetry breaking scale, the spacetime
structure is a regular hyperbola, however it becomes a charged black hole when
the magnitude of cosmological constant is less than the critical value. We
explain through duality transformation the reason why static global vortex
which is electrically neutral forms black hole with electric charge. Under the
present experimental bound of the cosmological constant, implications on
cosmology as a straight black cosmic string is also discussed in comparison
with global U(1) cosmic string in the spacetime of the zero cosmological
constant.Comment: 35 pages, Late
Gravitating Model Solitons
We study axially symmetric static solitons of O(3) nonlinear model
coupled to (2+1)-dimensional anti-de Sitter gravity. The obtained solutions are
not self-dual under static metric. The usual regular topological lump solution
cannot form a black hole even though the scale of symmetry breaking is
increased. There exist nontopological solitons of half integral winding in a
given model, and the corresponding spacetimes involve charged Baados-Teitelboim-Zanelli black holes without non-Abelian scalar hair.Comment: 35 pages, RevTe
The intrinsic shape of galaxy bulges
The knowledge of the intrinsic three-dimensional (3D) structure of galaxy
components provides crucial information about the physical processes driving
their formation and evolution. In this paper I discuss the main developments
and results in the quest to better understand the 3D shape of galaxy bulges. I
start by establishing the basic geometrical description of the problem. Our
understanding of the intrinsic shape of elliptical galaxies and galaxy discs is
then presented in a historical context, in order to place the role that the 3D
structure of bulges play in the broader picture of galaxy evolution. Our
current view on the 3D shape of the Milky Way bulge and future prospects in the
field are also depicted.Comment: Invited Review to appear in "Galactic Bulges" Editors: Laurikainen
E., Peletier R., Gadotti D. Springer Publishing. 24 pages, 7 figure
Free Energy of an Inhomogeneous Superconductor: a Wave Function Approach
A new method for calculating the free energy of an inhomogeneous
superconductor is presented. This method is based on the quasiclassical limit
(or Andreev approximation) of the Bogoliubov-de Gennes (or wave function)
formulation of the theory of weakly coupled superconductors. The method is
applicable to any pure bulk superconductor described by a pair potential with
arbitrary spatial dependence, in the presence of supercurrents and external
magnetic field. We find that both the local density of states and the free
energy density of an inhomogeneous superconductor can be expressed in terms of
the diagonal resolvent of the corresponding Andreev Hamiltonian, resolvent
which obeys the so-called Gelfand-Dikii equation. Also, the connection between
the well known Eilenberger equation for the quasiclassical Green's function and
the less known Gelfand-Dikii equation for the diagonal resolvent of the Andreev
Hamiltonian is established. These results are used to construct a general
algorithm for calculating the (gauge invariant) gradient expansion of the free
energy density of an inhomogeneous superconductor at arbitrary temperatures.Comment: REVTeX, 28 page
Observational Diagnostics of Gas Flows: Insights from Cosmological Simulations
Galactic accretion interacts in complex ways with gaseous halos, including
galactic winds. As a result, observational diagnostics typically probe a range
of intertwined physical phenomena. Because of this complexity, cosmological
hydrodynamic simulations have played a key role in developing observational
diagnostics of galactic accretion. In this chapter, we review the status of
different observational diagnostics of circumgalactic gas flows, in both
absorption (galaxy pair and down-the-barrel observations in neutral hydrogen
and metals; kinematic and azimuthal angle diagnostics; the cosmological column
density distribution; and metallicity) and emission (Lya; UV metal lines; and
diffuse X-rays). We conclude that there is no simple and robust way to identify
galactic accretion in individual measurements. Rather, progress in testing
galactic accretion models is likely to come from systematic, statistical
comparisons of simulation predictions with observations. We discuss specific
areas where progress is likely to be particularly fruitful over the next few
years.Comment: Invited review to appear in Gas Accretion onto Galaxies, Astrophysics
and Space Science Library, eds. A. J. Fox & R. Dave, to be published by
Springer. Typos correcte
Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model - I. Magnitude counts, redshift distribution, colour bimodality, and galaxy clustering
This paper presents a detailed comparison between high-redshift observations
from the VIMOS-VLT Deep Survey (VVDS) and predictions from the Munich
semi-analytical model of galaxy formation. In particular, we focus this
analysis on the magnitude, redshift, and colour distributions of galaxies, as
well as their clustering properties. We constructed 100 quasi-independent mock
catalogues, using the output of the semi-analytical model presented in De Lucia
& Blaizot (2007).We then applied the same observational selection function of
the VVDS-Deep survey, so as to carry out a fair comparison between models and
observations. We find that the semi-analytical model reproduces well the
magnitude counts in the optical bands. It tends, however, to overpredict the
abundance of faint red galaxies, in particular in the i' and z' bands. Model
galaxies exhibit a colour bimodality that is only in qualitative agreement with
the data. In particular, we find that the model tends to overpredict the number
of red galaxies at low redshift and of blue galaxies at all redshifts probed by
VVDS-Deep observations, although a large fraction of the bluest observed
galaxies is absent from the model. In addition, the model overpredicts by about
14 per cent the number of galaxies observed at 0.2<z<1 with I_AB<24. When
comparing the galaxy clustering properties, we find that model galaxies are
more strongly clustered than observed ones at all redshift from z=0.2 to z=2,
with the difference being less significant above z~1. When splitting the
samples into red and blue galaxies, we find that the observed clustering of
blue galaxies is well reproduced by the model, while red model galaxies are
much more clustered than observed ones, being principally responsible for the
strong global clustering found in the model. [abridged]Comment: 15 pages, 14 figures, accepted for publication in A&
Gas Accretion in Star-Forming Galaxies
Cold-mode gas accretion onto galaxies is a direct prediction of LCDM
simulations and provides galaxies with fuel that allows them to continue to
form stars over the lifetime of the Universe. Given its dramatic influence on a
galaxy's gas reservoir, gas accretion has to be largely responsible for how
galaxies form and evolve. Therefore, given the importance of gas accretion, it
is necessary to observe and quantify how these gas flows affect galaxy
evolution. However, observational data have yet to conclusively show that gas
accretion ubiquitously occurs at any epoch. Directly detecting gas accretion is
a challenging endeavor and we now have obtained a significant amount of
observational evidence to support it. This chapter reviews the current
observational evidence of gas accretion onto star-forming galaxies.Comment: Invited review to appear in Gas Accretion onto Galaxies, Astrophysics
and Space Science Library, eds. A. J. Fox & R. Dav\'e, to be published by
Springer. This chapter includes 22 pages with 7 Figure
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