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135
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 cosmologi-cal 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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cosmological black hole solutions are ob-tained by generalizing the expanding Kerr-Schild cosmological black holes to obtain the charged case, by performing a Kerr-Schild transformation of the Einstein-de Sitter universe (instead of a closed universe) to obtain non-expanding Kerr-Schild cosmo-logical black
Higher dimensional Kerr-Schild spacetimes
"... We investigate general properties of Kerr-Schild (KS) metrics in n> 4 spacetime dimensions. First, we show that the Weyl tensor is of type II or more special if the null KS vector k is geodetic (or, equivalently, if Tabk a k b = 0). We subsequently specialize to vacuum KS solutions, which natural ..."
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Cited by 16 (10 self)
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We investigate general properties of Kerr-Schild (KS) metrics in n> 4 spacetime dimensions. First, we show that the Weyl tensor is of type II or more special if the null KS vector k is geodetic (or, equivalently, if Tabk a k b = 0). We subsequently specialize to vacuum KS solutions, which
Regular Sources of the Kerr-Schild Class for Rotating and Nonrotating
- Black Hole Solutions ”, Phys. Rev.D65 (2002)064039, gr-qc/0109085
"... A unified approach to regular interiors of black holes with smooth matter distributions in the core region is given. The approach is based on a class of Kerr-Schild metrics representing minimal deformations of the Kerr-Newman solution, and allows us to give a common treatment for (charged and unchar ..."
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Cited by 7 (3 self)
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A unified approach to regular interiors of black holes with smooth matter distributions in the core region is given. The approach is based on a class of Kerr-Schild metrics representing minimal deformations of the Kerr-Newman solution, and allows us to give a common treatment for (charged
Black hole data via a Kerr-Schild approach”, Phys
- Rev. D
, 1998
"... We present a new approach for setting initial Cauchy data for multiple black hole spacetimes. The method is based upon adopting an initially Kerr-Schild form of the metric. In the case of non-spinning holes, the constraint equations take a simple hierarchical form which is amenable to direct numeric ..."
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Cited by 2 (0 self)
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We present a new approach for setting initial Cauchy data for multiple black hole spacetimes. The method is based upon adopting an initially Kerr-Schild form of the metric. In the case of non-spinning holes, the constraint equations take a simple hierarchical form which is amenable to direct
Gordon and Kerr–Schild ansätze in massive and bimetric gravity
, 2012
"... We develop the “generalized Gordon ansatz” for the ghost-free versions of both massive and bimetric gravity, an ansatz which is general enough to include almost all spacetimes commonly considered to be physically interesting, and restricted enough to greatly simplify calculations. The ansatz allows ..."
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Cited by 8 (0 self)
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– Schild ansatz ” can also be easily considered, now leading to an effective stress-energy tensor that corresponds to a null fluid. Cosmological implications are considered, as are consequences for black hole physics. Finally we have a few words to say concerning the null energy condition in the framework
Twisting Lightlike Solutions of the Kerr-Schild Class
, 2000
"... Using a complex representation of the Debney–Kerr–Schild (DKS) solutions and the Kerr theorem we give a method to construct boosted Kerr geometries. In the ultrarelativistic case this method yelds twisting solutions having, contrary to the known pp-wave limiting solutions, a non-zero value of the to ..."
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Using a complex representation of the Debney–Kerr–Schild (DKS) solutions and the Kerr theorem we give a method to construct boosted Kerr geometries. In the ultrarelativistic case this method yelds twisting solutions having, contrary to the known pp-wave limiting solutions, a non-zero value
Kerr-Schild Method and Geodesic Structure in Codimension-2 Brane Black Holes
"... We consider the black hole solutions of five-dimensional gravity with a Gauss-Bonnet term in the bulk and an induced gravity term on a 2-brane of codimension-2. Applying the Kerr-Schild method we derive additional solutions which include charge and angular momen-tum. To improve our understanding of ..."
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We consider the black hole solutions of five-dimensional gravity with a Gauss-Bonnet term in the bulk and an induced gravity term on a 2-brane of codimension-2. Applying the Kerr-Schild method we derive additional solutions which include charge and angular momen-tum. To improve our understanding
INTEGRAL EQUATIONS, KERR–SCHILD FIELDS AND GRAVITATIONAL SOURCES
, 2004
"... Kerr–Schild solutions to the vacuum Einstein equations are considered from the viewpoint of integral equations. We show that, for a class of Kerr–Schild fields, the stress-energy tensor can be regarded as a total divergence in Minkowski spacetime. If one assumes that Minkowski coordinates cover the ..."
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Cited by 2 (0 self)
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Kerr–Schild solutions to the vacuum Einstein equations are considered from the viewpoint of integral equations. We show that, for a class of Kerr–Schild fields, the stress-energy tensor can be regarded as a total divergence in Minkowski spacetime. If one assumes that Minkowski coordinates cover
Twistor String Structure of the Kerr-Schild Geometry and Consistency of the Dirac-Kerr System. ∗
, 812
"... Kerr-Schild (KS) geometry of the rotating black-holes and spinning particles is based on the associated with Kerr theorem twistor structure which is defined by an analytic curve F(Z) = 0 in the projective twistor space Z ∈ CP 3. On the other hand, there is a complex Newman representation which desc ..."
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Kerr-Schild (KS) geometry of the rotating black-holes and spinning particles is based on the associated with Kerr theorem twistor structure which is defined by an analytic curve F(Z) = 0 in the projective twistor space Z ∈ CP 3. On the other hand, there is a complex Newman representation which
Integral equations and Kerr-Schild fields II. The Kerr solution. Submitted to: Class. Quantum Grav
, 1997
"... Stationary vacuum solutions of Kerr-Schild type are analysed within the framework of gauge-theory gravity. The complex structure at the heart of these ¯elds is shown to have a clear geometric origin, with the role of the unit imaginary ful¯lled by the spacetime pseudoscalar. A number of general resu ..."
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Cited by 1 (1 self)
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Stationary vacuum solutions of Kerr-Schild type are analysed within the framework of gauge-theory gravity. The complex structure at the heart of these ¯elds is shown to have a clear geometric origin, with the role of the unit imaginary ful¯lled by the spacetime pseudoscalar. A number of general
Results 1 - 10
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