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Isofrequency pairing of geodesic orbits in Kerr geometry

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arxiv 1301.3918 v2 pith:BWIFBERT submitted 2013-01-16 gr-qc astro-ph.HE

Niels Warburton , Leor Barack , Norichika Sago This is my paper
classification gr-qcastro-ph.HE
keywords orbitssamethreeboundfrequenciesgeodesicisofrequencykerr
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Bound geodesic orbits around a Kerr black hole can be parametrized by three constants of the motion: the (specific) orbital energy, angular momentum and Carter constant. Generically, each orbit also has associated with it three frequencies, related to the radial, longitudinal and (mean) azimuthal motions. Here we note the curious fact that these two ways of characterizing bound geodesics are not in a one-to-one correspondence. While the former uniquely specifies an orbit up to initial conditions, the latter does not: there is a (strong-field) region of the parameter space in which pairs of physically distinct orbits can have the same three frequencies. In each such isofrequency pair the two orbits exhibit the same rate of periastron precession and the same rate of Lense-Thirring precession of the orbital plane, and (in a certain sense) they remain "synchronized" in phase.

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Cited by 2 Pith papers

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