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Abstract Cosmological Black Holes as Models of Cosmological Inhomogeneities
, 2006
"... Since cosmological black holes modify the density and pressure of the surrounding universe, and introduce heat conduction, they produce simple models of cosmological inhomogeneities that can be used to study the eect of inhomogeneities on the universe's expansion. In this thesis, new cosmologi ..."
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holes in asymptotically
at universes, and by performing a conformal transformation on isotropic black hole spacetimes to obtain isotropic cosmological black hole spacetimes. The latter approach is found to produce cosmological black holes with energymomentum tensors that are physical throughout
Bjorken expansion in the isotropic Kasner spacetime ∗
, 2009
"... An isotropic expansion for the QGP is proposed in curved Kasner spacetime for an experimental configuration with three dimensional set of beams. The fluid of relativistic particles has no shear viscosity but the nonzero bulk viscosity ζ is time dependent and its value could explain the enormous entr ..."
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Cited by 2 (0 self)
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An isotropic expansion for the QGP is proposed in curved Kasner spacetime for an experimental configuration with three dimensional set of beams. The fluid of relativistic particles has no shear viscosity but the nonzero bulk viscosity ζ is time dependent and its value could explain the enormous
Thermodynamics Of Black Holes
 In Antide Sitter
, 1983
"... One would expect spacetime to have a foamlike structure on the Planck scale with a very high topology. If spacetime is simply connected (which is assumed in this paper), the nontrivial homology occurs in dimension two, and spacetime can be regarded as being essentially the topological sum of S 2 × ..."
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Cited by 149 (0 self)
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× S 2 and K3 bubbles. Comparison with the instantons for pair creation of black holes shows that the S 2 × S 2 bubbles can be interpreted as closed loops of virtual black holes. It is shown that scattering in such topological fluctuations leads to loss of quantum coherence, or in other words, to a
Thermodynamics of spacetime: the Einstein equation of state
 Phys Rev Lett
, 1995
"... The Einstein equation is derived from the proportionality of entropy and horizon area together with the fundamental relation δQ = TdS connecting heat, entropy, and temperature. The key idea is to demand that this relation hold for all the local Rindler causal horizons through each spacetime point, w ..."
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Cited by 177 (7 self)
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, the Einstein equation is an equation of state. This perspective suggests that it may be no more appropriate to canonically quantize the Einstein equation than it would be to quantize the wave equation for sound in air. The four laws of black hole mechanics, which are analogous to those of thermodynamics, were
ON THE BLACK HOLE INTERIOR SPACETIME
, 2008
"... A new version of the geometry inside a black hole is proposed, on the grounds of an idea given by Doran et al. The spacetime is still time dependent and is a solution of Einstein’s equations with a stress tensor corresponding to an anisotropic fluid. The model leads to a timedependent cosmological ..."
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A new version of the geometry inside a black hole is proposed, on the grounds of an idea given by Doran et al. The spacetime is still time dependent and is a solution of Einstein’s equations with a stress tensor corresponding to an anisotropic fluid. The model leads to a timedependent cosmological
Black Holes in String Theory
"... This thesis is devoted to trying to find a microscopic quantum description of black holes. We consider black holes in string theory which is a quantum theory of gravity. We find that the “area law ” black hole entropy for extremal and nearextremal charged black holes arises from counting microscopi ..."
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Cited by 94 (1 self)
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microscopic configurations. We study black holes in five and four spacetime dimensions. We calculate the Hawking temperature and give a physical picture of the Hawking decay process.
On “manyblackhole” vacuum spacetimes
 Class. Quantum Grav
"... We prove that there are no restrictions on the spatial topology of asymptotically flat solutions of the vacuum Einstein equations in (n + 1)dimensions. We do this by gluing a solution of the vacuum constraint equations on an arbitrary compact manifold Σ n to an asymptotically Euclidean solution of ..."
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Cited by 19 (6 self)
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of the constraints on R n. For any Σ n which does not admit a metric of positive scalar curvature, this provides for the existence of asymptotically flat vacuum spacetimes with no maximal slices. Our main theorem is a special case of a more general gluing construction for nondegenerate solutions of the vacuum
Results 1  10
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