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Subjected to the tidal field of its companion, each component of a coalescingbinary suffers a slow change in its mass (tidal heating) and spin (tidaltorquing) during the inspiral and merger. For black holes, these changes areassociated with their absorption of energy and angular momentum fluxes. Thiseffect modifies the inspiral rate of the binary, and consequently, the phaseand amplitude of its gravitational waveform. Numerical relativity waveformscontain these effects inherently, whereas analytical approximants for the earlyinspiral phase have to include them manually in the energy balance equation. Inthis work, we construct a frequency-domain gravitational waveform model thatincorporates the effects of tidal heating of black holes. This is achieved byrecalibrating the inspiral phase of the waveform model IMRPhenomD toincorporate the phase corrections for tidal heating. We also includecorrections to the amplitude, but add them directly to the inspiral amplitudemodel of IMRPhenomD. We show that the new model is faithful, with less than 1%mismatch, against a set of hybrid waveforms, except for one outlier that barelybreaches this limit. The recalibrated model shows mismatches of up to $\sim16\%$ with IMRPhenomD for high mass ratios and spins. Amplitude correctionsbecome less significant for higher mass ratios, whereas the phase correctionsleave more impact - suggesting that the former is practically irrelevant forgravitational wave data analysis in Advanced LIGO (aLIGO), Virgo and KAGRA.Comparing with a set of 219 numerical relativity waveforms, we find that themedian of mismatches decreases by $\sim 4\%$ in aLIGO zero-detuned high powernoise curve, and by $\sim 2\%$ with a flat noise curve. This implies a modestbut notable improvement in waveform accuracy.

A phenomenological gravitational waveform model of binary black holes incorporating horizon fluxes