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We present IMRPhenomTPHM, a phenomenological model for the gravitational wavesignals emitted by the coalescence of quasi-circular precessing binary blackholes systems. The model is based on the "twisting up" approximation, whichmaps non-precessing signals to precessing ones in terms of a time dependentrotation described by three Euler angles, and which has been utilized inseveral frequency domain waveform models that have become standard tools ingravitational wave data analysis. Our model is however constructed in the timedomain, which allows several improvements over the frequency domain models: wedo not use the stationary phase approximation, we employ a simple approximationfor the precessing Euler angles for the ringdown signal, and we implement a newmethod for computing the Euler angles through the evolution of the spindynamics of the system, which is more accurate and also computationallyefficient.

New twists in compact binary waveform modelling: a fast time domain model for precession