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We report development of a code to calculate the scalar self-force on ascalar-charged particle moving on generic bound orbits in the Kerr spacetime.The scalar self-force model allows rapid development of computationaltechniques relevant to generic gravitational extreme-mass-ratio inspirals(EMRIs). Our frequency-domain calculations are made with arbitrary numericalprecision code written in \textsc{Mathematica}. We extend spectral sourceintegration techniques to the Kerr spacetime, increasing computationalefficiency. We model orbits with nearly arbitrary inclinations$0\leq\iota<\pi/2$ and eccentricities up to $e \lesssim 0.8$. This effortextends earlier work by Warburton and Barack where motion was restricted to theequatorial plane or to inclined spherical orbits. Consistent with a recentdiscovery by Thornburg and Wardell \cite{ThorWard17} in time-domaincalculations, we observe self-force oscillations during the radially-outboundportion of highly eccentric orbits around a rapidly rotating black hole. Asnoted previously, these oscillations reflect coupling into the self-force byquasinormal modes excited during pericenter passage. Our results confirm theeffect with a frequency-domain code. \emph{More importantly, we find thatquasinormal bursts (QNBs) appear directly in the waveform following eachperiastron passage.} These faint bursts are shown to be a superposition of theleast-damped overtone (i.e., fundamental) of at least four ($l=m \le 4$)quasinormal modes. Our results suggest that QNBs should appear in gravitationalwaveforms, and thus provide a gauge-invariant signal. Potentially observable inhigh signal-to-noise ratio EMRIs, QNBs would provide high-frequency componentsto the parameter estimation problem that would complement low-frequencyelements of the waveform.

physical review. d/physical review. d.

Repeated faint quasinormal bursts in extreme-mass-ratio inspiral  waveforms: Evidence from frequency-domain scalar self-force calculations on  generic Kerr orbits