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Change of sign of the velocity gradient (mesured with respect to locally non-rotating frames) has been found for accretion discs orbiting rapidly rotating Kerr black holes with spin a > 0.9953 for Keplerian discs [1] and a > 0.99979 for marginally stable thick discs [2]. Such “humpy” orbital velocity profiles occur close to but above the marginally stable circular geodesic of the black hole spacetimes. The maximal positive rate of change of the orbital velocity in terms of the proper radial distance introduces a locally defined critical frequency characterizing any processes in the disc capable to excite possible oscillations connected with the velocity hump. Comparing the “humpy frequency” related to distant observers with the epicyclic frequencies we show that in Keplerian discs orbiting extremely rapid Kerr holes (1− a 0.996 the resonant orbit r4:1 (with the ratio 4 : 1 between the vertical and radial epicyclic oscillations) occurs in the region of the hump. Applying the model on the nearly extreme black hole candidate GRS 1915+105, we conclude that for black hole parametersM = 14.8M⊙ and a= 0.9998 the observed high-frequency QPOs could be related to the hump-induced oscillations in thin accretion disc, as the first two QPOs, 41 Hz and 67 Hz, can be identified with the “humpy frequency” and the radial epicyclic frequency (at the same orbit). The other observed QPO-frequencies, 113 Hz and 166 Hz, can be explained as the combinational ones of the “humpy” and epicyclic frequencies.

Humpy LNRF-velocity profiles in accretion discs orbiting rapidly rotating Kerr black holes: a possible relation to QPOs