227 research outputs found
Regular black holes in an asymptotically de Sitter universe
A regular solution of the system of coupled equations of the nonlinear
electrodynamics and gravity describing static and spherically-symmetric black
holes in an asymptotically de Sitter universe is constructed and analyzed.
Special emphasis is put on the degenerate configurations (when at least two
horizons coincide) and their near horizon geometry. It is explicitly
demonstrated that approximating the metric potentials in the region between the
horizons by simple functions and making use of a limiting procedure one obtains
the solutions constructed from maximally symmetric subspaces with different
absolute values of radii. Topologically they are for the
cold black hole, when the event and cosmological horizon
coincide, and the Pleba\'nski- Hacyan solution for the ultraextremal black
hole. A physically interesting solution describing the lukewarm black holes is
briefly analyze
Intersecting black branes in strong gravitational waves
We consider intersecting black branes with strong gravitational waves
propagating along their worldvolume in the context of supergravity theories.
Both near-horizon and space-filling gravitational wave modes are included in
our ansatz. The equations of motion (originally, partial differential
equations) are shown to reduce to ordinary differential equations, which
include a Toda-like system. For special arrangements of intersecting black
branes, the Toda-like system becomes integrable, permitting a more thorough
analysis of the gravitational equations of motion.Comment: 17 pages; v2: cosmetic improvements, published versio
The Numerical Solution of Scalar Field for Nariai Case in 5D Ricci-flat SdS Black String Space with Polynomial Approximation
As one exact candidate of the higher dimensional black hole, the 5D
Ricci-flat Schwarzschild-de Sitter black string space presents something
interesting. In this paper, we give a numerical solution to the real scalar
field around the Nariai black hole by the polynomial approximation. Unlike the
previous tangent approximation, this fitting function makes a perfect match in
the leading intermediate region and gives a good description near both the
event and the cosmological horizons. We can read from our results that the wave
is close to a harmonic one with the tortoise coordinate. Furthermore, with the
actual radial coordinate the waves pile up almost equally near the both
horizons.Comment: 8 pages, 4 figure
Quantum Field Effects on Cosmological Phase Transition in Anisotropic Spacetimes
The one-loop renormalized effective potentials for the massive
theory on the spatially homogeneous models of Bianchi type I and
Kantowski-Sachs type are evaluated. It is used to see how the quantum field
affects the cosmological phase transition in the anisotropic spacetimes. For
reasons of the mathematical technique it is assumed that the spacetimes are
slowly varying or have specially metric forms. We obtain the analytic results
and present detailed discussions about the quantum field corrections to the
symmetry breaking or symmetry restoration in the model spacetimes.Comment: Latex 17 page
Uniqueness of Self-Similar Asymptotically Friedmann-Robertson-Walker Spacetime in Brans-Dicke theory
We investigate spherically symmetric self-similar solutions in Brans-Dicke
theory. Assuming a perfect fluid with the equation of state , we show that there are no non-trivial solutions which approach
asymptotically to the flat Friedmann-Robertson-Walker spacetime if the energy
density is positive. This result suggests that primordial black holes in
Brans-Dicke theory cannot grow at the same rate as the size of the cosmological
particle horizon.Comment: Revised version, 4 pages, no figures, Revtex, accepted for
publication in Physical Review
Deformed black strings in 5-dimensional Einstein-Yang-Mills theory
We construct the first examples of deformed non-abelian black strings in a
5-dimensional Einstein-Yang-Mills model. Assuming all fields to be independent
of the extra coordinate, we construct deformed black strings, which in the
4-dimensional picture correspond to axially symmetric non-abelian black holes
in gravity-dilaton theory. These solutions thus have deformed S^2 x R horizon
topology. We study fundamental properties of the black strings and find that
for all choices of the gravitational coupling two branches of solutions exist.
The limiting behaviour of the second branch of solutions however depends
strongly on the choice of the gravitational coupling.Comment: 8 Revtex pages; 4 eps figures; references adde
Cosmological Analogues of the Bartnik--McKinnon Solutions
We present a numerical classification of the spherically symmetric, static
solutions to the Einstein--Yang--Mills equations with cosmological constant
. We find three qualitatively different classes of configurations,
where the solutions in each class are characterized by the value of
and the number of nodes, , of the Yang--Mills amplitude. For sufficiently
small, positive values of the cosmological constant, \Lambda < \Llow(n), the
solutions generalize the Bartnik--McKinnon solitons, which are now surrounded
by a cosmological horizon and approach the deSitter geometry in the asymptotic
region. For a discrete set of values , the solutions are topologically --spheres, the ground state
being the Einstein Universe. In the intermediate region, that is for
\Llow(n) < \Lambda < \Lhig(n), there exists a discrete family of global
solutions with horizon and ``finite size''.Comment: 16 pages, LaTeX, 9 Postscript figures, uses epsf.st
Gravity on de-Sitter 3-Brane, Induced Einstein-Hilbert Term and Massless Gravitons
We study the extensions of DGP model which are described by five-dimensional
Einstein gravity coupled covariantly to 3-brane with induced gravity term and
consider warped D=4 de Sitter background field solutions on the brane. The case
with included D=5 AdS cosmological term is also considered. Following
background field method we obtain the field equations described by the
Lagrangean terms bilinear in gravitational field. In such a linear field
approximation on curved dS background we calculate explicitly the
five-dimensional massive terms as well as the mass-like ones on the brane. We
investigate the eigenvalue problem of Schr\"{o}dinger-like equation in fifth
dimension for graviton masses and discuss the existence of massless as well as
massive graviton modes in the bulk and on the brane without and with induced
gravity.Comment: LaTeX 26 pages, the version which appears in Class. Quant. Gra
Fully Explorable Horned Particles Hiding Charge
The charge-hiding effect by a horned particle, which was studied for the case
where gravity/gauge-field system is self-consistently interacting with a
charged lightlike brane (LLB) as a matter source, is now studied for the case
of a time like brane. From the demand that no surfaces of infinite coordinate
time redshift (horizons) appear in the problem we are lead now to a completly
explorable horned particle space for traveller that goes through the horned
particle (as was the case for the LLB) but now also in addition to this, the
horned region is fully visible to a static external observer. This requires
negative surface energy density for the shell sitting at the throat. We study a
gauge field subsystem which is of a special non-linear form containing a
square-root of the Maxwell term and which previously has been shown to produce
a QCD-like confining gauge field dynamics in flat space-time. The condition of
finite energy of the system or asymptotic flatness on one side of the horned
particle implies that the charged object sitting at the throat expels all the
flux it produces into the other side of the horned particle, which turns out to
be of a "tube-like" nature. An outside observer in the asymptotically flat
universe detects, therefore, apparently neutral object. The hiding of the
electric flux behind the tube-like region of a horned particle is the only
possible way that a truly charged particle can still be of finite energy, in a
theory that in flat space describes confinement. This points to the physical
relevance of such solutions, even though there is the need of negative energy
density at the throat of the horned particle, which can be of quantum
mechanical origin.Comment: The new version has been accepted for publication in Classical and
Quantum Gravity. Title changed to "Fully Explorable Horned Particles Hiding
Charge". Horned Particles terminology is used now instead of "wormholes" to
dscribe the solutions here. arXiv admin note: text overlap with
arXiv:1108.373
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