We study the description of Schwarzschild black holes, of entropy S, within matrix theory in the regime N > ∼ S ≫ 1. We obtain the most general matrix theory equation of state by requiring that black holes admit a description within this theory. It has a recognisable form in various cases. In some cases a D dimensional black hole can plausibly be thought of as a D̃ = D + 1 dimensional black hole...

from which the global properties can be understood. Here r(u, v) and w(u, v) are certain functions whose details are not so material. The important properties come from the singularities at uv = 1. There are two branches of this singularity, as u and v may be both negative or both positive. The “physical region” is the region uv < 1 between the two singularities. The branch of the singularity w...

1550-7998=20 We use the overlapping grids method to construct a fourth order accurate discretization of a first order reduction of the Klein-Gordon scalar field equation on a boosted spinning black hole background in axisymmetry. This method allows us to use a spherical outer boundary and excise the singularity from the domain with a spheroidal inner boundary which is moving with respect to the...

Beginning with Bekenstein, many authors have considered a uniformly spaced discrete quantum spectrum for black hole horizon area. It is also believed that the huge degeneracy of these area levels corresponds to the notion of black hole entropy. Starting from these two assumptions we here infer the algebra of a Schwarzschild black hole’s observables. This algebra then serves as motivation for in...

We discuss the stability of (charged) static black holes in higherdimensional spacetimes with and without cosmological constant by using gauge-invariant master equations of the Schrödinger equation type for black hole perturbations derived by the authors recently. In particular, we show that the stability of higher-dimensional Schwarzschild black holes can be proved with the help of a technique...

Employing energy-momentum pseudotensor of Einstein, we obtian the energy distribution of a dyonic dilaton black hole. The energy distribution of this black hole depends on mass M , electric charge Qe, magnetic charge Qm and asymptotic value of the dilaton φ0. We also make some comparisons between the results of Virbhadra et. al. and ours. PASC:04.20.-q, 04.50,+h E-mail:[email protected]...

A suggestion on how black holes may appear in Das-Jevicki Collective field theory is given. We study the behaviour of a ‘test’ particle when energy is sent into the system. A perturbation moving near the potential barrier can create a large-distance black hole geometry where the seeming curvature singularity is at the position of the barrier. In the simplest ‘static’ case the exact D = 2 black ...

We review the recently found map that takes any static and neutral Kaluza-Klein black hole, i.e. any static and neutral black hole on Minkowski-space times a circle Md × S1, and maps it to a corresponding solution for a nonand near-extremal brane on a circle. This gives a precise connection between phases of Kaluza-Klein black holes and the thermodynamic behavior of the non-gravitational theori...

We present new static spherically-symmetric exact solutions of Einstein equations with the quintessential matter surrounding a black hole charged or not as well as for the case without the black hole. A condition of additivity and linearity in the energy-momentum tensor is introduced, which allows one to get correct limits to the known solutions for the electromagnetic static field implying the...

We present new static spherically-symmetric exact solutions of Einstein equations with the quintessential matter surrounding a black hole charged or not as well as for the case without the black hole. A condition of additivity and linearity in the energy-momentum tensor is introduced, which allow one to get correct limits to the known solutions for the electromagnetic static field implying the ...