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    Orbital resonance model of QPOs in braneworld Kerr black hole spacetimes

    Zdeněk Stuchlík · Prosinec 01, 2007 · Fyzika · 0 comments
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    Publication date: Dec 2007

    Abstract:
    Rotating black holes in the brany universe of the Randall-Sundrum type
    with infinite additional dimension are described by the Kerr geometry
    with a tidal charge b representing the interaction of the brany black
    hole and the bulk spacetime. We investigate the role of the tidal charge
    in the orbital resonance model of quasiperiodic oscillations (QPOs) in
    black hole systems. The orbital Keplerian frequency ν_{K} and the radial
    and vertical epicyclic frequencies ν_{r}, ν_{θ} of the equatorial,
    quasicircular geodetical motion are discussed, and the local maxima of
    their radial profiles related to Keplerian accretion discs are given,
    assuming the inner edge of the disc located at loci of the innermost
    stable circular geodesic. The resonant conditions are given for possible
    direct (parametric) resonances of the oscillations with the radial and
    vertical epicyclic frequencies and for some trapped oscillations of the
    warped discs with resonant combinational frequencies involving the
    Keplerian and radial epicyclic frequencies. It is shown, how the tidal
    charge could influence matching of the observational data indicating the
    3:2 frequency ratio observed in GRS 1915+105 microquasar with prediction
    of the orbital resonance model. The „magic“ dimensionless black hole
    spin enabling presence of strong resonant phenomena at the radius, where
    ν_{K}:ν_{θ}:ν_{r} = 3:2:1, is determined in dependence on the tidal
    charge. Such strong resonances could be relevant even in sources with
    highly scattered resonant frequencies, as those expected in Sgr A*.

    Authors:
    Stuchlík, Zdeněk; Kotrlová, Andrea;

    https://ui.adsabs.harvard.edu/abs/2007ragt.meet..323S

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