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Privatization of irrigation schemes in New Zealand
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Ionospheric E-region Irregularities Produced by Non-linear Coupling of Unstable Plasma Waves
Ionospheric E region irregularities produced by nonlinear coupling of unstable plasma wave
Spin-2 Amplitudes in Black-Hole Evaporation
Quantum amplitudes for gravitational-wave perturbations of
Einstein/scalar collapse to a black hole are treated by analogy with
Maxwell perturbations. The spin-2 perturbations split into parts with odd and
even parity. We use the Regge-Wheeler gauge; at a certain point we make a gauge
transformation to an asymptotically-flat gauge, such that the metric
perturbations have the expected falloff behaviour at large radii. By analogy
with , for natural 'coordinate' variables are given by the magnetic
part of the Weyl tensor, which can be taken as boundary
data on a final space-like hypersurface . For simplicity, we take the
data on the initial surface to be exactly spherically-symmetric. The
(large) Lorentzian proper-time interval between and ,
measured at spatial infinity, is denoted by . We follow Feynman's
prescription and rotate into the complex: , for . The corresponding complexified {\it
classical} boundary-value problem is expected to be well-posed. The Lorentzian
quantum amplitude is recovered by taking the limit as . For
boundary data well below the Planck scale, and for a locally supersymmetric
theory, this involves only the semi-classical amplitude , where denotes the second-variation classical
action. The relations between the and natural boundary data,
involving supersymmetry, are investigated using 2-component spinor language in
terms of the Maxwell field strength and the Weyl spinor
Relic Radiation from an Evaporating Black Hole
We present a non-string-theoretic calculation of the microcanonical entropy
of relic integer-spin Hawking radiation -- at fixed total energy . The only
conserved macroscopic quantity is the total energy (the total energy of the
relic radiation). Data for a boundary-value approach, with massless,
integer-spin perturbations, are set on initial and final space-like
hypersurfaces. In the resulting 1-dimensional statistical-mechanics problem,
the real part of the (complex) time separation at spatial infinity, , is the variable conjugate to the total
energy. We count the number of weak-field configurations on the final
space-like hypersurface with energy . One recovers the Cardy formula and the
Bekenstein-Hawking entropy, if Re(T) is of the order of the black-hole life-
time, leading to a statistical interpretation of black-hole entropy. The
microcanonical entropy includes a logarithmic correction to the black-hole area
law, which is {\it universal} (independent of black-hole parameters). Here, the
discreteness of the energy levels is crucial. This approach is compared with
that of string theory for the transition to the fundamental-string r\'egime in
the final stages of evaporation. The squared coupling, , regulating the
transition to a highly-excited string state and {\it vice versa}, can be
related to the angle, , of complex-time rotation above. The
strong-coupling r\'egime corresponds to a Euclidean black hole, while the
physical limit of a Lorentzian space-time (as ) corresponds to
the weak-coupling r\'egime. This resembles the transition to a highly-excited
string-like state which subsequently decays into massless particles, thereby
avoiding the naked singularity.Comment: To appear in International Journal of Modern Physics
Black hole evaporation in a spherically symmetric non-commutative space-time
Recent work in the literature has studied the quantum-mechanical decay of a
Schwarzschild-like black hole, formed by gravitational collapse, into
almost-flat space-time and weak radiation at a very late time. The relevant
quantum amplitudes have been evaluated for bosonic and fermionic fields,
showing that no information is lost in collapse to a black hole. On the other
hand, recent developments in noncommutative geometry have shown that, in
general relativity, the effects of non-commutativity can be taken into account
by keeping the standard form of the Einstein tensor on the left-hand side of
the field equations and introducing a modified energy-momentum tensor as a
source on the right-hand side. Relying on the recently obtained
non-commutativity effect on a static, spherically symmetric metric, we have
considered from a new perspective the quantum amplitudes in black hole
evaporation. The general relativity analysis of spin-2 amplitudes has been
shown to be modified by a multiplicative factor F depending on a constant
non-commutativity parameter and on the upper limit R of the radial coordinate.
Limiting forms of F have been derived which are compatible with the adiabatic
approximation.Comment: 8 pages, Latex file with IOP macros, prepared for the QFEXT07
Conference, Leipzig, September 200
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