Disc formation from tidal disruption of stars on eccentric orbits by
  Kerr black holes using GRSPH
  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.
