37 research outputs found
Geodesic Deviation in the AdS Black String Spacetime
The equation of motion of test particles in the geometry of a black string
embedded in a 5-dimensional AdS spacetime is studied.Comment: 7 page
On the gravitational energy of the Hawking wormhole
The surface energy for a conformally flat spacetime which represents the
Hawking wormhole in spherical (static) Rindler coordinates is computed using
the Hawking - Hunter formalism for non asymptotically - flat spacetimes.
The physical gravitational Hamiltonian is proportional to the Rindler
acceleration g of the hyperbolic observer and is finite on the event horizon
ksi = b (b-the Planck length, ksi - the Minkowski interval). The corresponding
temperature of the system of particles associated to the massless scalar field
Psi, coupled conformally to Einstein's equations, is given by the Davies -
Unruh temperature up to a constant factor of order unity.Comment: 9 pages, chapter 4 removed, to appear in Int. Jour. Mod. Phys.
Does rotation generate a massive string ?
The properties of a stationary massive string endowed with intrinsic angular
momentum are investigated. The spacetime is generated by an "improper" time
translation combined with uniform rotation. The mass per unit length of the
string is proportional to the angular velocity . The spacetime is
Minkowskian geometrically but the topology is nontrivial thanks to the event
horizon located on the surface (similar with Rindler's spacetime) and
to the deficit angle generated by rotation. The Sagnac time delay is
calculated. It proves to be nonvanishing even when due to the
intrinsic spin of the string.Comment: 4 pages, minor changes, talk given at the XXIXth Spanish Relativity
Meeting (ERE 2006), Palma de Mallorca, Spain, Sept. 4 - 8, 2006, appeared in
Jour. Phys. : Conf. Ser. 66 (2007) 01205
Boundary sources in the Doran - Lobo - Crawford spacetime
We take a null hypersurface (the causal horizon) generated by a congruence of
null geodesics as the boundary of the Doran-Lobo-Crawford spacetime, to be the
place where the Brown-York quasilocal energy is located. The components of the
outer and inner stress tensors are computed and shown to depend on time and on
the impact parameter of the test particle trajectory. The surface energy
density on the boundary is given by the same expression as that
obtained previously for the energy stored on a Rindler horizon.Comment: 4 pages, title changed, no figures, minor text change
Thermodynamic Properties of Spherically-Symmetric, Uniformly-Accelerated Reference Frames
We aim to study the thermodynamic properties of the spherically symmetric
reference frames with uniform acceleration, including the spherically symmetric
generalization of Rindler reference frame and the new kind of uniformly
accelerated reference frame. We find that, unlike the general studies about the
horizon thermodynamics, one cannot obtain the laws of thermodynamics for their
horizons in the usual approaches, despite that one can formally define an area
entropy (Bekenstein-Hawking entropy). In fact, the common horizon for a set of
uniformly accelerated observers is not always exist, even though the
Hawking-Unruh temperature is still well-defined. This result indicates that the
Hawking-Unruh temperature is only a kinematic effect, to gain the laws of
thermodynamics for the horizon, one needs the help of dynamics. Our result is
in accordance with those from the various studies about the acoustic black
holes.Comment: 8 page
On the time dependent Schwarzschild - de Sitter spacetime
An imperfect cosmic fluid with energy flux is analyzed. Even though its
energy density is positive, the pressure due to the fact
that the metric is asymptotically de Sitter. The kinematical quantities for a
nongeodesic congruence are computed. The scalar expansion is time independent
but divergent at the singularity . Far from the central mass and
for a cosmic time , the heat flux does not depend on
Newton's constant .Comment: 8 pages, no figures, Sections 3 and 5 enlarged, one reference adde
A Note on Temperature and Energy of 4-dimensional Black Holes from Entropic Force
We investigate the temperature and energy on holographic screens for
4-dimensional black holes with the entropic force idea proposed by Verlinde. We
find that the "Unruh-Verlinde temperature" is equal to the Hawking temperature
on the horizon and can be considered as a generalized Hawking temperature on
the holographic screen outside the horizons. The energy on the holographic
screen is not the black hole mass but the reduced mass , which is
related to the black hole parameters. With the replacement of the black hole
mass by the reduced mass , the entropic force can be written as
, which could be tested by experiments.Comment: V4: 13 pages, 4 figures, title changed, discussions for experiments
added, accepted by CQ
Unwrapping Closed Timelike Curves
Closed timelike curves (CTCs) appear in many solutions of the Einstein
equation, even with reasonable matter sources. These solutions appear to
violate causality and so are considered problematic. Since CTCs reflect the
global properties of a spacetime, one can attempt to change its topology,
without changing its geometry, in such a way that the former CTCs are no longer
closed in the new spacetime. This procedure is informally known as unwrapping.
However, changes in global identifications tend to lead to local effects, and
unwrapping is no exception, as it introduces a special kind of singularity,
called quasi-regular. This "unwrapping" singularity is similar to the string
singularities. We give two examples of unwrapping of essentially 2+1
dimensional spacetimes with CTCs, the Gott spacetime and the Godel universe. We
show that the unwrapped Gott spacetime, while singular, is at least devoid of
CTCs. In contrast, the unwrapped Godel spacetime still contains CTCs through
every point. A "multiple unwrapping" procedure is devised to remove the
remaining circular CTCs. We conclude that, based on the two spacetimes we
investigated, CTCs appearing in the solutions of the Einstein equation are not
simply a mathematical artifact of coordinate identifications, but are indeed a
necessary consequence of General Relativity, provided only that we demand these
solutions do not possess naked quasi-regular singularities.Comment: 29 pages, 9 figure
Diamonds's Temperature: Unruh effect for bounded trajectories and thermal time hypothesis
We study the Unruh effect for an observer with a finite lifetime, using the
thermal time hypothesis. The thermal time hypothesis maintains that: (i) time
is the physical quantity determined by the flow defined by a state over an
observable algebra, and (ii) when this flow is proportional to a geometric flow
in spacetime, temperature is the ratio between flow parameter and proper time.
An eternal accelerated Unruh observer has access to the local algebra
associated to a Rindler wedge. The flow defined by the Minkowski vacuum of a
field theory over this algebra is proportional to a flow in spacetime and the
associated temperature is the Unruh temperature. An observer with a finite
lifetime has access to the local observable algebra associated to a finite
spacetime region called a "diamond". The flow defined by the Minkowski vacuum
of a (four dimensional, conformally invariant) quantum field theory over this
algebra is also proportional to a flow in spacetime. The associated temperature
generalizes the Unruh temperature to finite lifetime observers.
Furthermore, this temperature does not vanish even in the limit in which the
acceleration is zero. The temperature associated to an inertial observer with
lifetime T, which we denote as "diamond's temperature", is 2hbar/(pi k_b
T).This temperature is related to the fact that a finite lifetime observer does
not have access to all the degrees of freedom of the quantum field theory.Comment: One reference correcte
Quantization of the interior Schwarzschild black hole
We study a Hamiltonian quantum formalism of a spherically symmetric
space-time which can be identified with the interior of a Schwarzschild black
hole. The phase space of this model is spanned by two dynamical variables and
their conjugate momenta. It is shown that the classical Lagrangian of the model
gives rise the interior metric of a Schwarzschild black hole. We also show that
the the mass of such a system is a Dirac observable and then by quantization of
the model by Wheeler-DeWitt approach and constructing suitable wave packets we
get the mass spectrum of the black hole.Comment: 12 pages, 1 figure, revised versio