  We perform 1D/2D/3D relativistic hydrodynamical simulations of accretion
flows with low angular momentum, filling the gap between spherically symmetric
Bondi accretion and disc-like accretion flows. Scenarios with different
directional distributions of angular momentum of falling matter and varying
values of key parameters such as spin of central black hole, energy and angular
momentum of matter are considered. In some of the scenarios the shock front is
formed. We identify ranges of parameters for which the shock after formation
moves towards or outwards the central black hole or the long lasting
oscillating shock is observed. The frequencies of oscillations of shock
positions which can cause flaring in mass accretion rate are extracted. The
results are scalable with mass of central black hole and can be compared to the
quasi-periodic oscillations of selected microquasars (such as GRS 1915+105, XTE
J1550-564 or IGR J17091-3624), as well as to the supermassive black holes in
the centres of weakly active galaxies, such as Sgr $A^{*}$.
