Fig. 8.
Gravitational wave luminosity L for an object of mass μ in circular equatorial orbit around a Kerr BH of mass M and spin parameter a, as a function of the orbital radius r0. Each curve starts at the prograde ISCO radius of the corresponding value of a. The dotted curve corresponds to the quadrupole approximation as given by Eq. (31). The inset shows the relative difference with respect to the quadrupole formula (31) up to r0 = 50 M.
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