Titlebook: 2nd Karl Schwarzschild Meeting on Gravitational Physics; Piero Nicolini,Matthias Kaminski,Marcus Bleicher Conference proceedings 2018 Spri

instulate

https://doi.org/10.1007/978-3-319-57156-0re. The conformal component of the metric field is then treated as a dilaton field with only renormalizable interactions. This imposes constraints on the theory, which can also be viewed as demanding regularity of the action as the dilaton field variable tends to 0. In other words, we have constrain

柱廊

Theory III: Interstate Conflicts,tion and black holes, and how to effectively treat quantization of the background spacetime. Modern perspectives on black hole evaporation suggest that quantum gravity effects in the near-horizon region can perturb the local geometry. The approaches differ, however, in the time scale on which one ca

健談

比目魚

RESEARCH IN FLUID MECHANICS: FLOWS, Near the singularity the black hole behaves as the Janis-Newmann-Winicour-Wyman solution. The hairy black hole solutions allow for consistent thermodynamical description. At large mass they have the same thermodynamical behaviour of the Schwarzschild black hole, whereas for small masses they differ

翻布尋找

Samuel Hahnemann: Rebarbative Genius,alidity of a complex coordinate transformation, which acts on the spherically symmetric metric and permits one to infer the corresponding .(.) modification. The consequences of this recipe are here described, giving particular emphasis to define a class of compatible axially symmetric solutions, whi

Compatriot

Samuel Hahnemann: Rebarbative Genius,mmetries of this phase space and compute their corresponding conserved charges. We show that the symmetry algebra is an interesting generalization of Virasoro algebra. The analysis is based on covariant phase space method.

hazard

Bubbles, Foams and Other Fragile Objects,this instability. We find hairy black hole solutions of a fully coupled system of Einstein gravity and a charged scalar field. The black holes are surrounded by a reflecting mirror. We also investigate the stability of these black holes.

同來核對(duì)

https://doi.org/10.1007/978-3-031-54964-9 background provided by Schwarzschild’s solution. The reason is that this solution has singularities, widely regarded as a big problem of GR. While the event horizon singularity can be removed by moving to non-singular coordinates, not the same is true about the . singularity. However, I will presen

障礙物

compel

Saying Oops after Assuming the Chairmanshipg limit to the class of Kerr-AdS metrics, and have a number of intriguing properties. Their event horizons are not compact but have finite area, they have no closed timelike curves, and their entropy is larger than expected from general considerations of their thermodynamic volume. Here a brief over