60 research outputs found
Hawking Radiation as Tunneling: the D-dimensional rotating case
The tunneling method for the Hawking radiation is revisited and applied to
the dimensional rotating case. Emphasis is given to covariance of results.
Certain ambiguities afflicting the procedure are resolved.Comment: Talk delivered at the Seventh International Workshop Quantum Field
Theory under the influence of External Conditions, QFEXT'05, september
05,Barcelona, Spain. To appear in Journal of Phys.
On the semiclassical treatment of Hawking radiation
In the context of the semiclassical treatment of Hawking radiation we prove
the universality of the reduced canonical momentum for the system of a massive
shell self gravitating in a spherical gravitational field within the Painlev\'e
family of gauges. We show that one can construct modes which are regular on the
horizon both by considering as hamiltonian the exterior boundary term and by
using as hamiltonian the interior boundary term. The late time expansion is
given in both approaches and their time Fourier expansion computed to reproduce
the self reaction correction to the Hawking spectrum.Comment: 18 pages, LaTeX, Corrected typo
Problems with Tunneling of Thin Shells from Black Holes
It is shown that is not invariant under canonical
transformations in general. Specifically for shells tunneling out of black
holes, this quantity is not invariant under canonical transformations. It can
be interpreted as the transmission coefficient only in the cases in which it is
invariant under canonical transformations. Although such cases include alpha
decay, they do not include the tunneling of shells from black holes. The
simplest extension to this formula which is invariant under canonical
transformations is proposed. However it is shown that this gives half the
correct temperature for black holes.Comment: 25 pages, 3 figures; v4: Made changes for publicatio
Tunnelling through black rings
Hawking radiation of black ring solutions to 5-dimensional
Einstein-Maxwell-dilaton gravity theory is analyzed by use of the
Parikh-Wilczek tunnelling method. To get the correct tunnelling amplitude and
emission rate, we adopted and developed the Angheben-Nadalini-Vanzo-Zerbini
covariant approach to cover the effects of rotation and electronic discharge
all at once, and the effect of back reaction is also taken into account. This
constitute a unified approach to the tunnelling problem. Provided the first law
of thermodynamics for black rings holds, the emission rate is proportional to
the exponential of the change of Bekenstein-Hawking entropy. Explicit
calculation for black ring temperatures agree exactly with the results obtained
via the classical surface gravity method and the quasilocal formalism.Comment: 10 pages, V2: various modifications throughout the text, plus a lot
of newly added reference
Hawking Radiation as Tunneling for Extremal and Rotating Black Holes
The issue concerning semi-classical methods recently developed in deriving
the conditions for Hawking radiation as tunneling, is revisited and applied
also to rotating black hole solutions as well as to the extremal cases. It is
noticed how the tunneling method fixes the temperature of extremal black hole
to be zero, unlike the Euclidean regularity method that allows an arbitrary
compactification period. A comparison with other approaches is presented.Comment: 17 pages, Latex document, typos corrected, four more references,
improved discussion in section
Hamilton-Jacobi Tunneling Method for Dynamical Horizons in Different Coordinate Gauges
Previous work on dynamical black hole instability is further elucidated
within the Hamilton-Jacobi method for horizon tunneling and the reconstruction
of the classical action by means of the null-expansion method. Everything is
based on two natural requirements, namely that the tunneling rate is an
observable and therefore it must be based on invariantly defined quantities,
and that coordinate systems which do not cover the horizon should not be
admitted. These simple observations can help to clarify some ambiguities, like
the doubling of the temperature occurring in the static case when using
singular coordinates, and the role, if any, of the temporal contribution of the
action to the emission rate. The formalism is also applied to FRW cosmological
models, where it is observed that it predicts the positivity of the temperature
naturally, without further assumptions on the sign of the energy.Comment: Standard Latex document, typos corrected, refined discussion of
tunneling picture, subsection 5.1 remove
Fermions Tunnelling from Black Holes
We investigate the tunnelling of spin 1/2 particles through event horizons.
We first apply the tunnelling method to Rindler spacetime and obtain the Unruh
temperature. We then apply fermion tunnelling to a general non-rotating black
hole metric and show that the Hawking temperature is recovered.Comment: 22 pages, v2: added references, v3: fixed minor typos, v4: added a
new section applying fermion tunnelling method to Kruskal-Szekers
coordinates, fixed minor typo, and added references, v5: modified
introduction and conclusion, fixed typo
Tunnelling Methods and Hawking's radiation: achievements and prospects
The aim of this work is to review the tunnelling method as an alternative
description of the quantum radiation from black holes and cosmological
horizons. The method is first formulated and discussed for the case of
stationary black holes, then a foundation is provided in terms of analytic
continuation throughout complex space-time. The two principal implementations
of the tunnelling approach, which are the null geodesic method and the
Hamilton-Jacobi method, are shown to be equivalent in the stationary case. The
Hamilton-Jacobi method is then extended to cover spherically symmetric
dynamical black holes, cosmological horizons and naked singularities. Prospects
and achievements are discussed in the conclusions.Comment: Topical Review commissioned and accepted for publication by
"Classical and Quantum Gravity". 101 pages; 6 figure
Discontinuities in Scalar Perturbations of Topological Black Holes
We study the perturbative behaviour of topological black holes. We calculate
both analytically and numerically the quasi-normal modes of scalar
perturbations. In the case of small black holes we find discontinuities of the
quasi-normal modes spectrum at the critical temperature and we argue that this
is evidence of a second-order phase transition.Comment: 23 pages, 17 figures, published versio
Unruh--DeWitt detectors in spherically symmetric dynamical space-times
In the present paper, Unruh--DeWitt detectors are used in order to
investigate the issue of temperature associated with a spherically symmetric
dynamical space-times. Firstly, we review the semi-classical tunneling method,
then we introduce the Unruh--DeWitt detector approach. We show that for the
generic static black hole case and the FRW de Sitter case, making use of
peculiar Kodama trajectories, semiclassical and quantum field theoretic
techniques give the same standard and well known thermal interpretation, with
an associated temperature, corrected by appropriate Tolman factors. For a FRW
space-time interpolating de Sitter space with the Einstein--de Sitter universe
(that is a more realistic situation in the frame of CDM cosmologies),
we show that the detector response splits into a de Sitter contribution plus a
fluctuating term containing no trace of Boltzmann-like factors, but rather
describing the way thermal equilibrium is reached in the late time limit. As a
consequence, and unlike the case of black holes, the identification of the
dynamical surface gravity of a cosmological trapping horizon as an effective
temperature parameter seems lost, at least for our co-moving simplified
detectors. The possibility remains that a detector performing a proper motion
along a Kodama trajectory may register something more, in which case the
horizon surface gravity would be associated more likely to vacuum correlations
than to particle creation.Comment: 19 pages, to appear on IJTP. arXiv admin note: substantial text
overlap with arXiv:1101.525
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