Schwarzschild-de Sitter
Les bulles de masse négative dans un espace de de Sitter
... Donc pour faciliter leur aspect mathématique compliqué, considérons la description suivante : supposons que nous avons une bulle dont l’intérieur est défini par l’espace de De Sitter pure. Ce corps sphérique est ...
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Stabilité des bulles de masse négative dans un espace-temps de de Sitter
... de Sitter à l’intérieur et une géométrie de Schwarzschild-de Sitter à l’extérieur, il n’existe pas d’ensembles de paramètres tels que le potentiel de la bulle admet un minimum local et que la ...
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A geometry-preserving finite volume method for compressible fluids on Schwarzschild spacetime
... (a) Initial velocity (b) (c) (d) Figure 5.2.1. Propagation of a shock/rarefaction pattern (two schemes). To encompass other backgrounds (for instance, Schwarzschild-de Sitter spacetime, with cosmological ...
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The nonperturbative renormalization group for quantum field theory in de Sitter space
... de Sitter approach ...de Sitter is identical to the RG flow in Euclidean de Sitter which is eventually driven by a single degree of freedom, the zero mode of the compact ...
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Asymptotics of Solutions of the Wave Equation on de Sitter-Schwarzschild Space
... up at the corner, can always be blown down, the same is not true for temporal infinity. In fact, the ‘black hole end’ r = r bh resembles the ‘de Sitter end’ quite closely, which motivates the construction in the ...
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Weakly regular fluid flows with bounded variation on a Schwarzschild background
... that Schwarzschild spacetime is a spherically symmetric 1 solution to the vacuum Einstein equations of general relativity, and describes a massive body surrounded by a vacuum ...
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Static spherically symmetric Einstein-Vlasov bifurcations of the Schwarzschild spacetime
... ρ, p and p T are interpreted respectively as the energy density, the radial pressure and the tangential pressure. In order to construct solutions outside from the Schwarzschild black hole, the assumption ℓ 0 > ...
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Proper use of Schwarzschild Ledoux criteria in stellar evolution computations
... some codes use a wrong numerical scheme to locate the bound- aries of convective zones. In this paper we use the term semi-convective to refer to layers where the temperature gradient is in between the ...
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Inverse scattering at fixed energy for massive charged Dirac fields in de Sitter-Reissner-Nordström black holes
... for Schwarzschild (static, uncharged and spherically symmetric), (de Sitter)-Reissner-Nordstr¨ om (static, charged and spherically symmetric) and Kerr (uncharged and rotating) black holes was studied for ...
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Weakly regular fluid flows with bounded variation on the domain of outer communication of a Schwarzschild blackhole spacetime. A numerical study
... v t=20 Figure 7.2: Evolution of a perturbed steady shock, using the Glimm method Late-time behavior of general solutions It is obvious that the steady state solution satisfying (2.1) serves as a solution to the ...
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Direct and inverse scattering at fixed energy for massless charged Dirac fields by Kerr-Newman-de Sitter black holes
... The results of this Theorem are quite similar to the results obtained in [34, 15] in the setting of Kerr and Kerr-Newman black holes (Λ = 0 in our model). In particular, the absence of pure point spectrum for H is a ...
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Métriques prescrites sur le bord du coeur convexe d'une variété anti-de Sitter globalement hyperbolique maximale compacte de dimension trois
... 2.1.3 Constraint equations A GHMC anti-de Sitter spacetime is well defined if we know a Cauchy surface with enough data to allow us to reconstruct the whole manifold. Typically, those data are the induced metric ...
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Dominating surface group representations and deforming closed anti-de Sitter 3-manifolds
... then (σ◦j, σ◦ρ) is also admissible. Finally, for any g 1 , g 2 ∈ PSL(2, R), the pair (C g 1 ◦ j, C g 2 ◦ ρ) is still admissible (where C g i denotes the conjugation by g i on PSL(2, R)). We will denote by Adm(S) the ...
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Inverse scattering at fixed energy in de Sitter-Reissner-Nordström black holes
... In this paper, we consider massless Dirac fields propagating in the outer region of de Sitter- Reissner-Nordstr¨ om black holes. We show that the metric of such black holes is uniquely determined by the partial ...
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Schwarzschild-Tangherlini metric from scattering amplitudes in various dimensions
... We have shown how to reconstruct the classical Schwarzschild-Tangherlini metric from scattering amplitudes in four, five and six dimensions. We have extracted the classical contribution as defined in [ 12 ] from ...
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Inverse scattering in de Sitter-Reissner-Nordström black hole spacetimes
... In Section 4, we consider the case of nonzero cosmological constant Λ > 0, that is de Sitter-Reissner- Nordstr¨ om black holes and we have three unknown parameters M, Q, Λ a priori. The two asymptotic regions ...
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Decay and non-decay of the local energy for the wave equation in the De Sitter - Schwarzschild metric
... 1. Introduction There has been important progress in the question of local energy decay for the solution of the wave equation in black hole type space-times over the last years. The best results are now known in the ...
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Explicit formula and meromorphic extension of the resolvent for the massive Dirac operator in the Schwarzschild-Anti-de Sitter spacetime
... Kerr-de Sitter family of ...Kerr-de Sitter family by ...Kerr-Newman-de Sitter spacetime ...de Sitter-Reissner-Nordström black holes where an expansion in terms of resonances was ob- tained ...
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Quasimodes and a lower bound for the local energy decay of the Dirac equation in Schwarzschild-Anti-de Sitter spacetime
... the Schwarzschild black hole, we can see a tunneling effect where the probability of finding the particle in the classically forbidden region is exponentially ...
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Scattering theory for the Dirac equation on the Schwarzschild-Anti-de Sitter spacetime
... the Schwarzschild-AdS space-time with respect to spherically symmetric perturbations thanks to an exponential decay rate of the local energy ...the Schwarzschild-AdS black hole with arbitrary angular ...
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