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