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We present the results of relativistic smoothed particle hydrodynamicssimulations of tidal disruptions of stars by rotating supermassive black holes,for a wide range of impact parameters and black hole spins. For deepencounters, we find that: relativistic precession creates debris geometriesimpossible to obtain with the Newtonian equations; part of the fluid can belaunched on plunging orbits, reducing the fallback rate and the mass of theresulting accretion disc; multiple squeezings and bounces at periapsis maygenerate distinctive X-ray signatures resulting from the associated shockbreakout; disruptions can occur inside the marginally bound radius, if theangular momentum spread launches part of the debris on non-plunging orbits.Perhaps surprisingly, we also find relativistic effects important in partialdisruptions, where the balance between self-gravity and tidal forces is soprecarious that otherwise minor relativistic effects can have decisiveconsequences on the stellar fate. In between, where the star is fully disruptedbut relativistic effects are mild, the difference resides in a gentler rise ofthe fallback rate, a later and smaller peak, and longer return times. However,relativistic precession always causes thicker debris streams, both in the boundpart (speeding up circularization) and in the unbound part (accelerating andenhancing the production of separate transients). We discuss various propertiesof the disruption (compression at periapsis, shape and spread of the energydistribution) and potential observables (peak fallback rate, times of rise anddecay, duration of super-Eddington fallback) as a function of the impactparameter and the black hole spin.

Tidal disruptions by rotating black holes: effects of spin and impact parameter