Extended orbital resonance model with hump-induced oscillations

Details Extended orbital resonance model with hump-induced oscillations Extended orbital resonance model with hump-induced oscillations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ragt.meet..449s&link_type=abstract

Proceedings of RAGtime 8/9: Workshops on black holes and neutron stars, 15-19/19-21 September, 2006/2007, Hradec nad Moravicí, O

Physics

Black Hole Physics, Accretion, Accretion Disks, Relativity

Scientific paper

Change of sign of the LNRF-velocity gradient has been found for accretion discs orbiting rapidly rotating Kerr black holes with spin a > 0.9953 for Keplerian discs and a > 0.99979 for marginally stable thick discs. Such a "humpy" LNRF-velocity profiles occur just above the marginally stable circular geodesic and could be related to oscillations of accretion discs. The frequency of such "hump"-induced oscillations can be identified with the maximal rate of change of the orbital velocity within the "humpy" profile. Therefore, we introduce an extended orbital resonance model (EXORM) of quasiperiodic oscillations (QPOs) assuming non-linear resonant phenomena between oscillations with the orbital epicyclic frequencies and the humpy frequency defined in a fully general relativistic way. The EXORM is developed for both Keplerian discs and perfect-fluid tori where the approximation of oscillations with epicyclic frequencies is acceptable. Clearly, the EXORM could be applied to the near-extreme Kerr black hole systems exhibiting relatively complex QPO frequency patterns. Assuming a Keplerian disc, it can be shown that in the framework of the EXORM, all the QPOs observed in the microquasar GRS 1915+105 could be explained, while it is not possible in the case of QPOs observed in the Galactic Centre source Sgr A*.

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