Extended orbital resonance model applied to QPOs observed in three near-extreme Kerr black hole candidate systems

Details Extended orbital resonance model applied to QPOs observed in three near-extreme Kerr black hole candidate systems Extended orbital resonance model applied to QPOs observed in three near-extreme Kerr black hole candidate systems

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ragt.meet..257s&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, Relativity, Accretion, Accretion Discs, X-Rays: Individual: Grs 1915+105, Xte J1650-500, Ngc 5408 X-1

Scientific paper

The "Extended Orbital Resonance Model", i.e., the idea of oscillations induced by the hump of the orbital velocity profile (related to the locally non-rotating frames - LNRF), which are proposed to excite the oscillations of Keplerian discs around near-extreme Kerr black holes with epicyclic frequencies, is used to estimate the mass and spin of three near-extreme Kerr black hole candidates GRS 1915+105, XTE J1650-500, and NGC 5408 X-1. The hump-induced oscillations are characterized by the so-called "humpy frequency", and a non-linear resonant coupling between these and epicyclic oscillations is expected. It it shown that the quasiperiodic variability (QPOs) observed in these sources can be matched with the proposals of the model, giving for the mass and spin of their black holes values consistent with the other observationally-established estimates.

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