  We perform 3D general relativistic smoothed particle hydrodynamics (GRSPH)
simulations of tidal disruption events involving 1 $M_\odot$ stars and $10^6
M_\odot$ rotating supermassive black holes. We consider stars on initially
elliptical orbits both in, and inclined to, the black hole equatorial plane. We
confirm that stream-stream collisions caused by relativistic apsidal precession
rapidly circularise the disrupted material into a disc. For inclined
trajectories we find that nodal precession induced by the black hole spin (i.e.
Lense-Thirring precession) inhibits stream-stream collisions only in the first
orbit, merely causing a short delay in forming a disc, which is inclined to the
black hole equatorial plane. We also investigate the effect of radiative
cooling on the remnant disc structure. We find that with no cooling a thick,
extended, slowly precessing torus is formed, with a radial extent of 5 au (for
orbits with a high penetration factor). Radiatively efficient cooling produces
a narrow, rapidly precessing ring close to pericentre. We plot the energy
dissipation rate, which tracks the pancake shock, stream-stream collisions and
viscosity. We compare this to the effective luminosity due to accretion onto
the black hole. We find energy dissipation rates of $\sim10^{45}$ erg s$^{-1}$
for stars disrupted at the tidal radius, and up to $\sim10^{47}$ erg s$^{-1}$
for deep encounters.
