  We consider the motion of nonspinning, compact objects orbiting around a Kerr
black hole with tidal couplings. The tide-induced quadrupole moment modifies
both the orbital energy and outgoing fluxes, so that over the inspiral
timescale there is an accumulative shift in the orbital and gravitational wave
phase. Previous studies on compact object tidal effects have been carried out
in the Post-Newtonian (PN) and Effective-One-Body (EOB) formalisms. In this
work, within the black hole perturbation framework, we propose to characterize
the tidal influence in the expansion of mass ratios, while higher-order PN
corrections are naturally included. For the equatorial and circular orbit, we
derive the leading order, frequency dependent tidal phase shift which agrees
with the Post-Newtonian result at low frequencies but deviates at high
frequencies. We also find that such phase shift has weak dependence ($\le
10\%$) on the spin of the primary black hole. Combining this black hole
perturbation waveform with the Post-Newtonian waveform, we propose a
frequency-domain, hybrid waveform that shows comparable accuracy as the EOB
waveform in characterizing the tidal effects, as calibrated by numerical
relativity simulations. Further improvement is expected as the next-leading
order in mass ratio and the higher-PN tidal corrections are included. This
hybrid approach is also applicable for generating binary black hole waveforms.
