35 research outputs found
Quantum Ergoregion Instability
We have shown that, as in the case of black holes, an ergosphere itself with
no event horizon inside can evaporate spontaneously, giving energy radiation to
spatial infinity until the ergoregion disappears. However, the feature of his
quantum ergoregion instability is very much different from black hole
radiation. It is rather analogous to a laser amplification. This analysis is
based on the canonical quantization of a neutral scalar field in the presence
of unstable modes characterized by complex frequencies in a simple model for a
rapidly rotating star.Comment: 10 pages, latex, one epsfig, to appear in the Proceedings of the
APCTP Winter School on Duality of String Theory, Korea, Feb. 17-28, 1997; a
brief version of gr-qc/9701040 with slightly different presentatio
Evaporation of large black holes in AdS: greybody factor and decay rate
We consider a massless, minimally coupled scalar field propagating through
the geometry of a black 3-brane in an asymptotically space.
The wave equation for modes traveling purely in the holographic direction
reduces to a Heun equation and the corresponding greybody factor is obtained
numerically. Approximations valid in the low- and high-frequency regimes are
also obtained analytically. The greybody factor is then used to determine the
rate of evaporation of these large black holes in the context of the evaporon
model proposed in \cite{Rocha:2008fe}. This setting represents the evolution of
a black hole under Hawking evaporation with a known CFT dual description and is
therefore unitary. Information must then be preserved under this evaporation
process.Comment: 20 pages, 2 figures; v2: added references, published versio
Towers of Gravitational Theories
In this essay we introduce a theoretical framework designed to describe black
hole dynamics. The difficulties in understanding such dynamics stems from the
proliferation of scales involved when one attempts to simultaneously describe
all of the relevant dynamical degrees of freedom. These range from the modes
that describe the black hole horizon, which are responsible for dissipative
effects, to the long wavelength gravitational radiation that drains mechanical
energy from macroscopic black hole bound states. We approach the problem from a
Wilsonian point of view, by building a tower of theories of gravity each of
which is valid at different scales. The methodology leads to multiple new
results in diverse topics including phase transitions of Kaluza-Klein black
holes and the interactions of spinning black hole in non-relativistic orbits.
Moreover, our methods tie together speculative ideas regarding dualities for
black hole horizons to real physical measurements in gravitational wave
detectors.Comment: Awarded second prize for 2006 Gravity Research Foundation essay
contes
Charge and mass effects on the evaporation of higher-dimensional rotating black holes
To study the dynamics of discharge of a brane black hole in TeV gravity
scenarios, we obtain the approximate electromagnetic field due to the charged
black hole, by solving Maxwell's equations perturbatively on the brane. In
addition, arguments are given for brane metric corrections due to backreaction.
We couple brane scalar and brane fermion fields with non-zero mass and charge
to the background, and study the Hawking radiation process using well known low
energy approximations as well as a WKB approximation in the high energy limit.
We argue that contrary to common claims, the initial evaporation is not
dominated by fast Schwinger discharge.Comment: Published version. Minor typos corrected. 29 pages, 5 figure
Damping of Tensor Modes in Cosmology
An analytic formula is given for the traceless transverse part of the
anisotropic stress tensor due to free streaming neutrinos, and used to derive
an integro-differential equation for the propagation of cosmological
gravitational waves. The solution shows that anisotropic stress reduces the
squared amplitude by 35.6 % for wavelengths that enter the horizon during the
radiation-dominated phase, independent of any cosmological parameters. This
decreases the tensor temperature and polarization correlation functions for
these wavelengths by the same amount. The effect is less for wavelengths that
enter the horizon at later times. At the longest wavelengths the decrease in
the tensor correlation functions due to neutrino free streaming ranges from
10.7% for to 9.0% for . An Appendix gives a
general proof that tensor as well as scalar modes satisfy a conservation law
for perturbations outside the horizon, even when the anisotropic stress tensor
is not negligible.Comment: 14 pages. The original version of this paper has been expanded to
deal with perturbations of any wavelength. While for wavelengths short enough
to enter the horizon during radiation dominance, temperature and polarization
correlations are damped by 35.6%, at the longest wavelengths the damping is
from 9.0% to 11%. An added Appendix gives a general proof that tensor as well
as scalar modes satisfy a conservation law outside the horizon, even during
neutrino decoupling. Some references are also adde
Quantum Vacuum Instability Near Rotating Stars
We discuss the Starobinskii-Unruh process for the Kerr black hole. We show
how this effect is related to the theory of squeezed states. We then consider a
simple model for a highly relativistic rotating star and show that the
Starobinskii-Unruh effect is absent.Comment: 17 Pages, (accepted by PRD), (previously incorrect header files have
been corrected
The Primordial Gravitational Wave Background in String Cosmology
We find the spectrum P(w)dw of the gravitational wave background produced in
the early universe in string theory. We work in the framework of String Driven
Cosmology, whose scale factors are computed with the low-energy effective
string equations as well as selfconsistent solutions of General Relativity with
a gas of strings as source. The scale factor evolution is described by an early
string driven inflationary stage with an instantaneous transition to a
radiation dominated stage and successive matter dominated stage. This is an
expanding string cosmology always running on positive proper cosmic time. A
careful treatment of the scale factor evolution and involved transitions is
made. A full prediction on the power spectrum of gravitational waves without
any free-parameters is given. We study and show explicitly the effect of the
dilaton field, characteristic to this kind of cosmologies. We compute the
spectrum for the same evolution description with three differents approachs.
Some features of gravitational wave spectra, as peaks and asymptotic
behaviours, are found direct consequences of the dilaton involved and not only
of the scale factor evolution. A comparative analysis of different treatments,
solutions and compatibility with observational bounds or detection perspectives
is made.Comment: LaTeX, 50 pages with 2 figures. Uses epsfig and psfra
CBR Anisotropy and the Running of the Scalar Spectral Index
Accurate () predictions for the anisotropy of the Cosmic
Background Radiation (CBR) are essential for using future high-resolution
() CBR maps to test cosmological models. In many inflationary
models the variation (``running'') of the spectral index of the spectrum of
density perturbations is a significant effect and leads to changes of around
1\% to 10\% in the CBR power spectrum. We propose a general method for taking
running into account which uses the derivative of the spectral index (). Conversely, high-resolution CBR maps may be able to determine ,
giving important information about the inflationary potential.Comment: Discussion of calculation clarified; error corrected which reduces
estimated effect for chaotic inflatio
One loop renormalization of the four-dimensional theory for quantum dilaton gravity.
We study the one loop renormalization in the most general metric-dilaton
theory with the second derivative terms only. The general theory can be divided
into two classes, models of one are equivalent to conformally coupled with
gravity scalar field and also to general relativity with cosmological term. The
models of second class have one extra degree of freedom which corresponds to
dilaton. We calculate the one loop divergences for the models of second class
and find that the arbitrary functions of dilaton in the starting action can be
fine-tuned in such a manner that all the higher derivative counterterms
disappear on shell. The only structures in both classical action and
counterterms, which survive on shell, are the potential (cosmological) ones.
They can be removed by renormalization of the dilaton field which acquire the
nontrivial anomalous dimension, that leads to the effective running of the
cosmological constant. For some of the renormalizable solutions of the theory
the observable low energy value of the cosmological constant is small as
compared with the Newtonian constant. We also discuss another application of
our result.Comment: 21 pages, latex, no figures
Curing singularities in cosmological evolution of F(R) gravity
We study modified gravity models which are capable of driving the
accelerating epoch of the Universe at the present time whilst not destroying
the standard Big Bang and inflationary cosmology. Recent studies have shown
that a weak curvature singularity with can arise generically in
viable models of present dark energy (DE) signaling an internal
incompleteness of these models. In this work we study how this problem is cured
by adding a quadratic correction with a sufficiently small coefficient to the
function at large curvatures. At the same time, this correction
eliminates two more serious problems of previously constructed viable DE
models: unboundedness of the mass of a scalar particle (scalaron) arising in
gravity and the scalaron overabundance problem. Such carefully
constructed models can also yield both an early time inflationary epoch and a
late time de Sitter phase with vastly different values of . The reheating
epoch in these combined models of primordial and present dark energy is
completely different from that of the old inflationary
model, mainly due to the fact that values of the effective gravitational
constant at low and intermediate curvatures are different for positive and
negative . This changes the number of e-folds during the observable part of
inflation that results in a different value of the primordial power spectrum
index.Comment: Discussion expanded, references added, results unchanged, accepted
for publication in JCAP. A minor typo in Eq. (2.14) has been correcte