Abstract. We obtain a fourth order accurate numerical algorithm to integrate the Zerilli and Regge-Wheeler wave equations, describing perturbations of nonrotating black holes, with source terms due to an orbiting particle. Those source terms contain the Dirac’s delta and its first derivative. We also re-derive the source of the Zerilli and Regge-Wheeler equations for more convenient definitions...

where AH is the area of a black hole surface and lP = (h̄G/c) is the Planck length [1, 2]. In black hole physics the Bekenstein-Hawking entropy S plays essentially the same role as in the usual thermodynamics. In particular it allows to estimate what part of the internal energy of a black hole can be transformed into work. Four laws of black hole physics that form the basis in the thermodynamica...

The entropy of a BTZ black hole in the presence of gravitational Chern-Simons terms has previously been analyzed using Euclidean action formalism. In this paper we treat the BTZ solution as a two dimensional black hole by regarding the angular coordinate as a compact direction, and use Wald’s Noether charge method to calculate the entropy of this black hole in the presence of higher derivative ...

This is the users manual of the black-hole event generator BlackMax [1], which simulates the experimental signatures of microscopic and Planckian black-hole production and evolution at protonproton, proton-antiproton and electron-positron colliders in the context of brane world models with low-scale quantum gravity. The generator is based on phenomenologically realistic models free of serious p...

The central black-hole masses of a sample of 30 luminous quasars are estimated using Hβ fwhm measurements from a combination of new and previously-published nuclear spectra. The quasar black-hole mass estimates are combined with reverberationmapping measurements for a sample of Seyfert galaxies (Wandel, Peterson & Malkan 1999) in order to study AGN black-hole masses over a wide range in nuclear...

Black holes of mass M must have a spin angular momentum S below the Kerr limit ( S=M 1), but whether astrophysical black holes can attain this limiting spin depends on their accretion history. Gas accretion from a thin disk limits the black-hole spin to gas & 0:9980 0:0002, as electromagnetic radiation from this disk with retrograde angular momentum is preferentially absorbed by the black hole....

B holes are among the strangest predictions of Einstein’s general theory of relativity: regions of spacetime in which gravity is so strong that nothing—not even light—can escape. More precisely, a black hole is a singularity in spacetime surrounded by an event horizon, a surface that acts as a perfect one-way membrane: matter and radiation can enter the event horizon, but, once inside, can neve...

The quantum string emission by Black Holes is computed in the framework of the “string analogue model” (or thermodynamical approach), which is well suited to combine QFT and string theory in curved backgrounds (particulary here, as black holes and strings posses intrinsic thermal features and temperatures). The QFT-Hawking temperature TH is upper bounded by the string temperature TS in the blac...

The quantum black hole model with a self-gravitating spherically symmetric thin dust shell as a source is considered. The shell Hamiltonian constraint is written and the corresponding Schroedinger equation is obtained. This equation appeared to be a finite differences equation. Its solutions are required to be analytic functions on the relevant Riemannian surface. The method of finding discrete...

According to the thermodynamical analogy in black hole physics, the entropy of a black hole in the Einstein theory of gravity equals S BH = A H /(4l 2 P), where A H is the area of a black hole surface and l P = (¯ hG/c 3) 1/2 is the Planck length [1, 2]. In black hole physics the Bekenstein-Hawking entropy S BH plays essentially the same role an in the usual thermodynamics. In particular it all...