  We investigate relativistic low angular momentum accretion of inviscid
perfect fluid onto a Schwarzschild black hole. The simulations are performed
with a general-relativistic, high-resolution (second-order), shock-capturing,
hydrodynamical numerical code. We use horizon-penetrating Eddington-Finkelstein
coordinates to remove inaccuracies in regions of strong gravity near the black
hole horizon and show the expected convergence of the code with the Michel
solution and stationary Fishbone-Moncrief toroids. We recover, in the framework
of relativistic hydrodynamics, the qualitative behavior known from previous
Newtonian studies that used a Bondi background flow in a pseudo-relativistic
gravitational potential with a latitude-dependent angular momentum at the outer
boundary. Our models exhibit characteristic "turbulent" behavior and the
attained accretion rates are lower than those of the Bondi-Michel radial flow.
For sufficiently low values of the asymptotic sound speed, geometrically thick
tori form in the equatorial plane surrounding the black hole horizon while
accretion takes place mainly through the poles.
