12 research outputs found
The Rotating Quantum Thermal Distribution
We show that the rigidly rotating quantum thermal distribution on flat
space-time suffers from a global pathology which can be cured by introducing a
cylindrical mirror if and only if it has a radius smaller than that of the
speed-of-light cylinder. When this condition is met, we demonstrate numerically
that the renormalized expectation value of the energy-momentum stress tensor
corresponds to a rigidly rotating thermal bath up to a finite correction except
on the mirror where there are the usual Casimir divergences.Comment: 8 pages, 2 PostScript figure
Tidal invariants for compact binaries on quasicircular orbits
We extend the gravitational self-force approach to encompass "self-interaction" tidal effects for a compact body of mass Ό on a quasicircular orbit around a black hole of mass M=Ό. Specifically, we define and calculate at O(Ό) (conservative) shifts in the eigenvalues of the electric- and magnetic-type tidal tensors, and a (dissipative) shift in a scalar product between their eigenbases. This approach yields four gauge-invariant functions, from which one may construct other tidal quantities such as the curvature scalars and the speciality index. First, we analyze the general case of a geodesic in a regular perturbed vacuum spacetime admitting a helical Killing vector and a reflection symmetry. Next, we specialize to focus on circular orbits in the equatorial plane of Kerr spacetime at O(Ό). We present accurate numerical results for the Schwarzschild case for orbital radii up to the light ring, calculated via independent implementations in Lorenz and Regge-Wheeler gauges. We show that our results are consistent with leading-order post-Newtonian expansions, and demonstrate the existence of additional structure in the strong-field regime. We anticipate that our strong-field results will inform (e.g.) effective one-body models for the gravitational two-body problem that are invaluable in the ongoing search for gravitational waves
Octupolar invariants for compact binaries on quasicircular orbits
We extend the gravitational self-force methodology to identify and compute new O(Ό) tidal invariants for a compact body of mass Ό on a quasicircular orbit about a black hole of mass MΌ. In the octupolar sector we find seven new degrees of freedom, made up of 3+3 conservative/dissipative 'electric' invariants and 3+1 'magnetic' invariants, satisfying 1+1 and 1+0 trace conditions. We express the new invariants for equatorial circular orbits on Kerr spacetime in terms of the regularized metric perturbation and its derivatives; and we evaluate the expressions in the Schwarzschild case. We employ both Lorenz gauge and Regge-Wheeler gauge numerical codes, and the functional series method of Mano, Suzuki and Takasugi. We present (i) highly-accurate numerical data and (ii) high-order analytical post-Newtonian expansions. We demonstrate consistency between numerical and analytical results, and prior work. We explore the application of these invariants in effective one-body models and binary black hole initial-data formulations
Motion of Inertial Observers Through Negative Energy
Recent research has indicated that negative energy fluxes due to quantum
coherence effects obey uncertainty principle-type inequalities of the form
|\Delta E|\,{\Delta \tau} \lprox 1\,. Here is the magnitude of
the negative energy which is transmitted on a timescale . Our main
focus in this paper is on negative energy fluxes which are produced by the
motion of observers through static negative energy regions. We find that
although a quantum inequality appears to be satisfied for radially moving
geodesic observers in two and four-dimensional black hole spacetimes, an
observer orbiting close to a black hole will see a constant negative energy
flux. In addition, we show that inertial observers moving slowly through the
Casimir vacuum can achieve arbitrarily large violations of the inequality. It
seems likely that, in general, these types of negative energy fluxes are not
constrained by inequalities on the magnitude and duration of the flux. We
construct a model of a non-gravitational stress-energy detector, which is
rapidly switched on and off, and discuss the strengths and weaknesses of such a
detector.Comment: 18pp + 1 figure(not included, available on request), in LATEX,
TUPT-93-
Quantum Radiation from a 5-Dimensional Rotating Black Hole
We study a massless scalar field propagating in the background of a
five-dimensional rotating black hole. We showed that in the Myers-Perry metric
describing such a black hole the massless field equation allows the separation
of variables. The obtained angular equation is a generalization of the equation
for spheroidal functions. The radial equation is similar to the radial
Teukolsky equation for the 4-dimensional Kerr metric. We use these results to
quantize the massless scalar field in the space-time of the 5-dimensional
rotating black hole and to derive expressions for energy and angular momentum
fluxes from such a black hole.Comment: references added, accepted for publication in Physical Review
Some general properties of the renormalized stress-energy tensor for static quantum states on (n+1)-dimensional spherically symmetric black holes
We study the renormalized stress-energy tensor (RSET) for static quantum
states on (n+1)-dimensional, static, spherically symmetric black holes. By
solving the conservation equations, we are able to write the stress-energy
tensor in terms of a single unknown function of the radial co-ordinate, plus
two arbitrary constants. Conditions for the stress-energy tensor to be regular
at event horizons (including the extremal and ``ultra-extremal'' cases) are
then derived using generalized Kruskal-like co-ordinates. These results should
be useful for future calculations of the RSET for static quantum states on
spherically symmetric black hole geometries in any number of space-time
dimensions.Comment: 9 pages, no figures, RevTeX4, references added, accepted for
publication in General Relativity and Gravitatio
Linear dilaton black holes
We present new solutions to Einstein-Maxwell-dilaton-axion (EMDA) gravity in
four dimensions describing black holes which asymptote to the linear dilaton
background. In the non-rotating case they can be obtained as the limiting
geometry of dilaton black holes. The rotating solutions (possibly endowed with
a NUT parameter) are constructed using a generating technique based on the
Sp(4,R) duality of the EMDA system. In a certain limit (with no event horizon
present) our rotating solutions coincide with supersymmetric
Israel-Wilson-Perjes type dilaton-axion solutions. In presence of an event
horizon supersymmetry is broken. The temperature of the static black holes is
constant, and their mass does not depend on it, so the heat capacity is zero.
We investigate geodesics and wave propagation in these spacetimes and find
superradiance in the rotating case. Because of the non-asymptotically flat
nature of the geometry, certain modes are reflected from infinity, in
particular, all superradiant modes are confined. This leads to classical
instability of the rotating solutions. The non-rotating linear dilaton black
holes are shown to be stable under spherical perturbations.Comment: 30 pages, 1 eps figure, 8 typos correcte
Detector Description and Performance for the First Coincidence Observations between LIGO and GEO
For 17 days in August and September 2002, the LIGO and GEO interferometer
gravitational wave detectors were operated in coincidence to produce their
first data for scientific analysis. Although the detectors were still far from
their design sensitivity levels, the data can be used to place better upper
limits on the flux of gravitational waves incident on the earth than previous
direct measurements. This paper describes the instruments and the data in some
detail, as a companion to analysis papers based on the first data.Comment: 41 pages, 9 figures 17 Sept 03: author list amended, minor editorial
change
Black Holes at the LHC
In these two lectures, we will address the topic of the creation of small
black holes during particle collisions in a ground-based accelerator, such as
LHC, in the context of a higher-dimensional theory. We will cover the main
assumptions, criteria and estimates for their creation, and we will discuss
their properties after their formation. The most important observable effect
associated with their creation is likely to be the emission of Hawking
radiation during their evaporation process. After presenting the mathematical
formalism for its study, we will review the current results for the emission of
particles both on the brane and in the bulk. We will finish with a discussion
of the methodology that will be used to study these spectra, and the observable
signatures that will help us identify the black-hole events.Comment: 37 pages, 14 figures, lectures presented in the 4th Aegean Summer
School on Black Holes, 17-22 September 2007, Lesvos, Greece, typos corrected,
comments and references adde
Finite aspects of quantum field theory on curved space-time
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