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    Mass and Spin Estimates OT Two Near-Extreme Kerr Black Hole Candidates GRS 1915+105 and XTE J1650-500 from the Extended Orbital Resonance Model for High-Frequency Qpos

    Zdeněk Stuchlík · Leden 01, 2012 · Fyzika · 0 comments
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    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;

    https://ui.adsabs.harvard.edu/abs/2012mgm..conf..934S

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