A G Nicholson, B J Addis, H Bharucha, C A Clelland, B Corrin, A R Gibbs, P S Hasleton, K M Kerr, N B N Ibrahim, S Stewart, W A H Wallace, A U Wells . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ....

Using thermal quantization of geodesics confined under horizons and reasonable conjecture on massless modes, we evaluate quantum spectrum of Kerr black hole masses compatible with superstring symmetries.

We have obtained the correct expression for the centrifugal force acting on a particle at the equatorial circumference of a rotating body in the locally non-rotating frame of the Kerr geometry. Using this expression for the equilibrium of an element on the surface of a slowly rotating Maclaurin spheroid, we obtain the expression for the ellipticity (as discussed earlier by Abramowicz and Miller...

In the Randall-Sundrum two-brane model (RS1), a Kerr black hole on the brane can be naturally identified with a section of rotating black string. To estimate KaluzaKlein (KK) corrections on gravitational waves emitted by perturbed rotating black strings, we give the effective Teukolsky equation on the brane which is separable equation and hence numerically manageable. In this process, we derive...

The existence of supermassive collapsed objects in the cores of most galaxies poses still-unanswered questions. First, how did they form, and how does their mass depend on the properties of the host galaxy? Second, can observations probe the metric in the strong-field domain, testing whether it indeed agrees with the Kerr geometry predicted by general relativity (and, if so, what the spin is)?

As oil and gas exploration moves into deeper offshore areas, Shallow Water Flow (SWF) from overpressured, unconsolidated/uncemented sands becomes a high profile drilling hazard. Laboratory measurements show that SWF sands have high seismic compressional to shear velocity (Vp/Vs) ratios. Thus, elastic seismic inversion for Vp/Vs provides a quantitative identification of SWF sands, and predrill p...

We calculate the structure of accretion disc around a rapidly rotating black hole with a super-Eddington accretion rate. The luminosity and height of the disc are reduced by the advection effect. In the case of a large viscosity parameter, α > 0.03, the accretion flow strongly deviates from thermodynamic equilibrium and overheats in the central region. With increasing accretion rate, the flow t...

The capture or scattering of an initially straight infinite test cosmic string by a Kerr-Newman black hole, or by any other small source of an electrovac gravitational field, is analyzed analytically when the string moves with initial velocity v 0 and large impact parameter z 0 = b ≫ M so that the string stays very nearly straight (except during the final capture process, if that occurs, or exc...

Download Massive complex scalar field in the Kerr–Sen geometry: Exact solution of wave equation and Hawking radiation S. Q. Wu Interdisciplinary Center for Theoretical Study, and Department of Astronomy and Applied Physics, University of Science and Technology, Hefei 230026, People’s Republic of China and Institute of Particle Physics, Hua-Zhong Normal University, Wuhan 430079, People’s Republi...

We derive the system of equations describing the time dependent twisted accretion disc around a Kerr black hole (twist equations). The post-Newtonian corrections to the equations of motion and effects of the gravitomagnetic force are taken into account. We show that introduction of appropriate coordinate system greatly simplifies the derivation of equations and allows to consider sufficiently l...