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The disruption of a star by the tidal forces of a spinning black hole causesthe stellar stream to precess affecting the conditions for triggering the tidaldisruption event (TDE). In this work, we study the effect that precessionimprints on TDE light curves due to the interaction of the TDE wind andluminosity with the stream wrapped around the black hole. We performtwo-dimensional radiation-hydrodynamic simulations using the moving-meshhydrodynamic code JET with its radiation treatment module. We study the impactof black hole mass, accretion efficiency, and inclination between the orbitaland spin planes. From our results, we identified two behaviours: $i)$ modelswith low-mass black holes ($M_\text{h}\sim10^6~\text{M}_{\odot}$), lowinclination ($i\sim0$), and low accretion efficiency ($\eta\sim0.01$) showlight curves with a short early peak caused by the interaction of the wind withthe inner edge of the stream. The line of sight has little effect on the lightcurve, since the stream covers a small fraction of the solid angle due to theprecession occurring in the orbital plane; $ii)$ models with high-mass blackholes ($M_\text{h}\gtrsim10^7~\text{M}_{\odot}$), high inclination($i\sim90^{\circ}$), and high accretion efficiency ($\eta\sim0.1$) producelight curves with luminosity peaks that can be delayed by up to 50-100 ddepending on the line of sight due to presence of the precessed stream blockingthe radiation in the early phase of the event. Our results show that black holespin and misalignment do not imprint recognisable features on the light curvesbut rather can add complications to their analysis.

The effect of relativistic precession on light curves of tidal disruption events