92 research outputs found
Covariant anomaly and Hawking radiation from the modified black hole in the rainbow gravity theory
Recently, Banerjee and Kulkarni (R. Banerjee, S. Kulkarni, arXiv:0707.2449
[hep-th]) suggested that it is conceptually clean and economical to use only
the covariant anomaly to derive Hawking radiation from a black hole. Based upon
this simplified formalism, we apply the covariant anomaly cancellation method
to investigate Hawking radiation from a modified Schwarzschild black hole in
the theory of rainbow gravity. Hawking temperature of the gravity's rainbow
black hole is derived from the energy-momentum flux by requiring it to cancel
the covariant gravitational anomaly at the horizon. We stress that this
temperature is exactly the same as that calculated by the method of cancelling
the consistent anomaly.Comment: 5 page
Anomaly analysis of Hawking radiation from Kaluza-Klein black hole with squashed horizon
Considering gravitational and gauge anomalies at the horizon, a new method
that to derive Hawking radiations from black holes has been developed by
Wilczek et al. In this paper, we apply this method to non-rotating and rotating
Kaluza-Klein black holes with squashed horizon, respectively. For the rotating
case, we found that, after the dimensional reduction, an effective U(1) gauge
field is generated by an angular isometry. The results show that the gauge
current and energy-momentum tensor fluxes are exactly equivalent to Hawking
radiation from the event horizon.Comment: 15 pages, no figures, the improved version, accepted by Eur. Phys. J.
Black Hole Entropy: From Shannon to Bekenstein
In this note we have applied directly the Shannon formula for information
theory entropy to derive the Black Hole (Bekenstein-Hawking) entropy. Our
analysis is semi-classical in nature since we use the (recently proposed [8])
quantum mechanical near horizon mode functions to compute the tunneling
probability that goes in to the Shannon formula, following the general idea of
[5]. Our framework conforms to the information theoretic origin of Black Hole
entropy, as originally proposed by Bekenstein.Comment: 9 pages Latex, Comments are welcome; Thoroughly revised version,
reference and acknowledgements sections enlarged, numerical error in final
result corrected, no major changes, to appear in IJT
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
Remarks on Hawking radiation as tunneling from the BTZ black holes
Hawking radiation viewed as a semiclassical tunneling process from the event
horizon of the (2 + 1)-dimensional rotating BTZ black hole is carefully
reexamined by taking into account not only the energy conservation but also the
conservation of angular momentum when the effect of the emitted particle's
self-gravitation is incorporated. In contrast to previous analysis of this
issue in the literature, our result obtained here fits well to the
Kraus-Parikh-Wilczek's universal conclusion without any modification to the
Bekenstein-Hawking area-entropy formulae of the BTZ black hole.Comment: 12pages, no figure, use JHEP3.cls. Version better than published one
in JHE
G\"{o}del black hole, closed timelike horizon, and the study of particle emissions
We show that a particle, with positive orbital angular momentum, following an
outgoing null/timelike geodesic, shall never reach the closed timelike horizon
(CTH) present in the -dimensional rotating G\"{o}del black hole
space-time. Therefore a large part of this space-time remains inaccessible to a
large class of geodesic observers, depending on the conserved quantities
associated with them. We discuss how this fact and the existence of the closed
timelike curves present in the asymptotic region make the quantum field
theoretic study of the Hawking radiation, where the asymptotic observer states
are a pre-requisite, unclear. However, the semiclassical approach provides an
alternative to verify the Smarr formula derived recently for the rotating
G\"{o}del black hole. We present a systematic analysis of particle emissions,
specifically for scalars, charged Dirac spinors and vectors, from this black
hole via the semiclassical complex path method.Comment: 13 pages; minor changes, references adde
Quantum corrections to the entropy of charged rotating black holes
Hawking radiation from a black hole can be viewed as quantum tunneling of
particles through the event horizon. Using this approach we provide a general
framework for studying corrections to the entropy of black holes beyond
semiclassical approximations. Applying the properties of exact differentials
for three variables to the first law thermodynamics, we study charged rotating
black holes and explicitly work out the corrections to entropy and horizon area
for the Kerr-Newman and charged rotating BTZ black holes. It is shown that the
results for other geometries like the Schwarzschild, Reissner-Nordstr\"{o}m and
anti-de Sitter Schwarzschild spacetimes follow easily
Corrections to Hawking-like Radiation for a Friedmann-Robertson-Walker Universe
Recently, a Hamilton-Jacobi method beyond semiclassical approximation in
black hole physics was developed by \emph{Banerjee} and
\emph{Majhi}\cite{beyond0}. In this paper, we generalize their analysis of
black holes to the case of Friedmann-Robertson-Walker (FRW) universe. It is
shown that all the higher order quantum corrections in the single particle
action are proportional to the usual semiclassical contribution. The
corrections to the Hawking-like temperature and entropy of apparent horizon for
FRW universe are also obtained. In the corrected entropy, the area law involves
logarithmic area correction together with the standard inverse power of area
term.Comment: 10 pages, no figures, comments are welcome; v2: references added and
some typoes corrected, to appear in Euro.Phys.J.C; v3:a defect corrected. We
thank Dr.Elias Vagenas for pointing out a defect of our pape
Thermodynamics Inducing Massive Particles' Tunneling and Cosmic Censorship
By calculating the change of entropy, we prove that the first law of black
hole thermodynamics leads to the tunneling probability of massive particles
through the horizon, including the tunneling probability of massive charged
particles from the Reissner-Nordstr\"om black hole and the Kerr-Newman black
hole. Novelly, we find the trajectories of massive particles are close to that
of massless particles near the horizon, although the trajectories of massive
charged particles may be affected by electromagnetic forces. We show that
Hawking radiation as massive particles tunneling does not lead to violation of
the weak cosmic-censorship conjecture
Spectroscopy of the Einstein-Maxwell-Dilaton-Axion black hole
The entropy spectrum of a spherically symmetric black hole was derived via
the Bohr-Sommerfeld quantization rule in Majhi and Vagenas's work. Extending
this work to charged and rotating black holes, we quantize the horizon area and
the entropy of an Einstein-Maxwell-Dilaton-Axion (EMDA) black hole via the
Bohr-Sommerfeld quantization rule and the adiabatic invariance. The result
shows the area spectrum and the entropy spectrum are respectively equally
spaced and independent on the parameters of the black hole.Comment: 9 page
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