1,338 research outputs found
Where are all the gravastars? Limits upon the gravastar model from accreting black holes
The gravastar model, which postulates a strongly correlated thin shell of
anisotropic matter surrounding a region of anti-de Sitter space, has been
proposed as an alternative to black holes. We discuss constraints that
present-day observations of well-known black hole candidates place on this
model. We focus upon two black hole candidates known to have extraordinarily
low luminosities: the supermassive black hole in the Galactic Center,
Sagittarius A*, and the stellar-mass black hole, XTE J1118+480. We find that
the length scale for modifications of the type discussed in Chapline et al.
(2003) must be sub-Planckian.Comment: 11 pages, 4 figure
Advances and limitations in the modelling of fabricated photonic bandgap fibers
Copyright © 2006 IEEEWe model fabricated silica photonic bandgap fibers and achieve good agreement between simulated and measured properties. We identify the size of the SEM bitmap image as the ultimate limit to the accurate calculation of surfaces modes within the bandgapF. Poletti, M. N. Petrovich, R. Amezcua-Correa, N. G. Broderick, T. M. Monro and D. J. Richardsonhttp://eprints.soton.ac.uk/47883
Brillouin suppression through longitudinal structural variation in high nonlinearity silica holey fibers
Copyright © 2006 IEEEWe consider longitudinal variation in the fiber structure as a method of increasing the Brillouin linewidth and threshold within high nonlinearity silica holey fibers. Strategies to control the associated variation in nonlinearity and dispersion along the fiber length are described.http://www.ofcnfoec.org/materials/06AbstractsWednesday.pd
Double Exchange Model for Magnetic Hexaborides
A microscopic theory for rare-earth ferromagnetic hexaborides, such as
Eu(1-x)Ca(x)B6, is proposed on the basis of the double-exchange Hamiltonian. In
these systems, the reduced carrier concentrations place the Fermi level near
the mobility edge, introduced in the spectral density by the disordered spin
background. We show that the transport properties such as Hall effect,
magnetoresitance, frequency dependent conductivity, and DC resistivity can be
quantitatively described within the model. We also make specific predictions
for the behavior of the Curie temperature, Tc, as a function of the plasma
frequency, omega_p.Comment: 4 pages, 3 figure
Theory of Nonlinear Dispersive Waves and Selection of the Ground State
A theory of time dependent nonlinear dispersive equations of the Schroedinger
/ Gross-Pitaevskii and Hartree type is developed. The short, intermediate and
large time behavior is found, by deriving nonlinear Master equations (NLME),
governing the evolution of the mode powers, and by a novel multi-time scale
analysis of these equations. The scattering theory is developed and coherent
resonance phenomena and associated lifetimes are derived. Applications include
BEC large time dynamics and nonlinear optical systems. The theory reveals a
nonlinear transition phenomenon, ``selection of the ground state'', and NLME
predicts the decay of excited state, with half its energy transferred to the
ground state and half to radiation modes. Our results predict the recent
experimental observations of Mandelik et. al. in nonlinear optical waveguides
Can accretion disk properties distinguish gravastars from black holes?
Gravastars, hypothetic astrophysical objects, consisting of a dark energy
condensate surrounded by a strongly correlated thin shell of anisotropic
matter, have been proposed as an alternative to the standard black hole picture
of general relativity. Observationally distinguishing between astrophysical
black holes and gravastars is a major challenge for this latter theoretical
model. In the context of stationary and axially symmetrical geometries, a
possibility of distinguishing gravastars from black holes is through the
comparative study of thin accretion disks around rotating gravastars and
Kerr-type black holes, respectively. In the present paper, we consider
accretion disks around slowly rotating gravastars, with all the metric tensor
components estimated up to the second order in the angular velocity. Due to the
differences in the exterior geometry, the thermodynamic and electromagnetic
properties of the disks (energy flux, temperature distribution and equilibrium
radiation spectrum) are different for these two classes of compact objects,
consequently giving clear observational signatures. In addition to this, it is
also shown that the conversion efficiency of the accreting mass into radiation
is always smaller than the conversion efficiency for black holes, i.e.,
gravastars provide a less efficient mechanism for converting mass to radiation
than black holes. Thus, these observational signatures provide the possibility
of clearly distinguishing rotating gravastars from Kerr-type black holes.Comment: 12 pages, 12 figures. V2: 14 pages, significant discussion and
references added, to appear in Class.Quant.Gra
Dense stellar matter with trapped neutrinos under strong magnetic fields
We investigate the effects of strong magnetic fields on the equation of state
of dense stellar neutrino-free and neutrino-trapped matter. Relativistic
nuclear models both with constant couplings (NLW) and with density dependent
parameters (DDRH) and including hyperons are considered . It is shown that at
low densities neutrinos are suppressed in the presence of the magnetic field.
The magnetic field reduces the strangeness fraction of neutrino-free matter and
increases the strangeness fraction of neutrino-trapped matter. The mass-radius
relation of stars described by these equations of state are determined. The
magnetic field makes the overall equation of state stiffer and the stronger the
field the larger the mass of maximum mass star and the smaller the baryon
density at the center of the star. As a consequence in the presence of strong
magnetic fields the possibility that a protoneutron star evolves to a blackhole
is smaller.Comment: 18 pages, 13 figures, 5 tables, submitted to J. Phys.
Gravastar energy conditions revisited
We consider the gravastar model where the vacuum phase transition between the
de Sitter interior and the Schwarzschild or Schwarzschild-de Sitter exterior
geometries takes place at a single spherical delta-shell. We derive sharp
analytic bounds on the surface compactness (2m/r) that follow from the
requirement that the dominant energy condition (DEC) holds at the shell. In the
case of Schwarzschild exterior, the highest surface compactness is achieved
with the stiff shell in the limit of vanishing (dark) energy density in the
interior. In the case of Schwarzschild-de Sitter exterior, in addition to the
gravastar configurations with the shell under surface pressure, gravastar
configurations with vanishing shell pressure (dust shells), as well as
configurations with the shell under surface tension, are allowed by the DEC.
Respective bounds on the surface compactness are derived for all cases. We also
consider the speed of sound on the shell as derived from the requirement that
the shell is stable against the radial perturbations. The causality requirement
(sound speed not exceeding that of light) further restricts the space of
allowed gravastar configurations.Comment: LaTeX/IOP-style, 16 pages, 2 figures, changes wrt v1: motivation for
eq. (6) clarified, several referecnes added (to appear in Class. Quantum
Grav.
Radial stability analysis of the continuous pressure gravastar
Radial stability of the continuous pressure gravastar is studied using the
conventional Chandrasekhar method. The equation of state for the static
gravastar solutions is derived and Einstein equations for small perturbations
around the equilibrium are solved as an eigenvalue problem for radial
pulsations. Within the model there exist a set of parameters leading to a
stable fundamental mode, thus proving radial stability of the continuous
pressure gravastar. It is also shown that the central energy density possesses
an extremum in rho_c(R) curve which represents a splitting point between stable
and unstable gravastar configurations. As such the rho_c(R) curve for the
gravastar mimics the famous M(R) curve for a polytrope. Together with the
former axial stability calculations this work completes the stability problem
of the continuous pressure gravastar.Comment: 17 pages, 5 figures, References corrected, minor changes wrt v1,
matches published versio
How to tell a gravastar from a black hole
Gravastars have been recently proposed as potential alternatives to explain
the astrophysical phenomenology traditionally associated to black holes,
raising the question of whether the two objects can be distinguished at all.
Leaving aside the debate about the processes that would lead to the formation
of a gravastar and the astronomical evidence in their support, we here address
two basic questions: Is a gravastar stable against generic perturbations? If
stable, can an observer distinguish it from a black hole of the same mass? To
answer these questions we construct a general class of gravastars and determine
the conditions they must satisfy in order to exist as equilibrium solutions of
the Einstein equations. For such models we perform a systematic stability
analysis against axial-perturbations, computing the real and imaginary parts of
the eigenfrequencies. Overall, we find that gravastars are stable to axial
perturbations, but also that their quasi-normal modes differ from those of a
black hole of the same mass and thus can be used to discern, beyond dispute, a
gravastar from a black hole.Comment: 16 pages, 13 figures, minor improvemen
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