7 Generalized Smarr formula for mass on the Cauchy horizon In this section we will derive for a stationary state black hole spacetime that the entropy can be expressed as S±=E±2T± on the H±, where T± is the Hawking temperature on H± and E± is shown to be the Komar energy on...
Theoretical or Mathematical/ black holesgeneral relativitygravitation/ mass formulasurface stressesAbraham-Lorentz electrongeneral relativityelectromagnetic origingravitational radiusstatic quasi-black hole/ A0470 Physics of black holes A0420 General relativity A0455 Alternative theories of gravitation...
P. Ramadevi, in Encyclopedia of Mathematical Physics, 2006 BTZ Black Hole and Its Partition Function Only for negative Λ we have a black hole solution of the Einstein’s equations. This solution, known as the BTZ black hole (Carlip 2003), in Euclidean gravity is given by the metric d...
A Schwarzschild Black Hole is defined as a region in space where the gravitational field is so strong that light cannot escape, resulting in a singularity at the Schwarzschild radius. AI generated definition based on: Special Relativity, Electrodynamics, and General Relativity (Second Edition), 2018...
We identify the origin of these terms in the macroscopic formula for the black hole entropy, based on quantum entropy function, as the contribution from non-trivial saddle point(s) in the path integral of string theory over the near horizon geometry. These saddle points exist only when the ...
Black Hole Uniqueness Theorems: Scalar mappings This timely review provides a self-contained introduction to the mathematical theory of stationary black holes and a self-consistent exposition of the corresponding uniqueness theorems. The opening chapters examine the general properties... M Heusler 被引量...
Several black hole configurations with Schrödinger asymp- totics have been reported in the literature. Some of them were derived within string and M-theory through the Melviniza- tion method. Different black hole seed solutions with a fixed critical exponent and dimension have been treated; the...
home to Einstein from 1933 until his death in 1955. The problem is that an equation for a black hole’s mass goes to infinity in a mathematical representation of spacetime, which models three-dimensional space plus time. That’s called a singularity, and “nature doesn’t like singularities,...
In the proof of this proposition we obtain a similar formula (F.40) for the coefficientsW_nappearing in the inverse relation (5.5). Of course, the function (5.48) must be equal to (5.32), which is guaranteed by the fact that they are solutions of Vignéras’ equation with the same as...
, respectively. we consider the problem of gluing the initial data of a small asymptotically flat black hole (such as a schwarzschild or kerr black hole with small mass), or more generally of a rescaled asymptotically flat initial data set \((\mathbb {r}^n\setminus {\hat{k}}^\circ ,{...