Publication date: Jan 2012
Abstract:
Humpy profile of the LNRF-related orbital velocity was found for
accretion discs orbiting rapidly rotating Kerr black holes with a spin a
> 0.9953 (Keplerian discs) and a > 0.99979 (marginally stable
thick discs). Maximal positive rate of change of the orbital velocity in
terms of the proper radial distance is used to define a local frequency
characterising possible physical processes in the disc connected with
the velocity hump. Comparing the „humpy frequency“ related to distant
observers with epicyclic frequencies of perturbed orbital motion, it was
shown that in Keplerian discs orbiting near-extreme Kerr black holes (a
> 0.998) the the ratio of radial epicyclic frequency and humpy
frequency (both evaluated at the same radius) is in terms of small
integers asymptotically going to the ratio 3:2 for a → 1. The Extended
Orbital Resonance Model with non-linear hump-induced oscillations was
applied to two X-ray variable sources GRS 1915+105 and XTE J1650-500. In
the case of GRS 1915+105, the model is able to address the whole set of
reported QPOs, giving the mass and spin of the central black hole: a =
0.9998; M = 14:8M☉. For XTE J1650-500, similar ideas give
values a = 0.9982; M = 5:1M☉.
Authors:
Slaný, Petr; Stuchlík, Zdeněk;