  We perform hydro- and magnetohydrodynamical general relativistic simulations
of a tidal disruption of a $0.1\,M_\odot$ red dwarf approaching a
$10^5\,M_\odot$ non-rotating massive black hole on a close (impact parameter
$\beta=10$) elliptical (eccentricity $e=0.97$) orbit. We track the debris
self-interaction, circularization, and the accompanying accretion through the
black hole horizon. We find that the relativistic precession leads to the
formation of a self-crossing shock. The dissipated kinetic energy heats up the
incoming debris and efficiently generates a quasi-spherical outflow. The
self-interaction is modulated because of the feedback exerted by the flow on
itself. The debris quickly forms a thick, almost marginally bound disc that
remains turbulent for many orbital periods. Initially, the accretion through
the black hole horizon results from the self-interaction, while in the later
stages it is dominated by the debris originally ejected in the shocked region,
as it gradually falls back towards the hole. The effective viscosity in the
debris disc stems from the original hydrodynamical turbulence, which dominates
over the magnetic component. The radiative efficiency is very low because of
low energetics of the gas crossing the horizon and large optical depth that
results in photon trapping.
