  The recent ALMA maps together with observations of H$_2$O maser emission seem
to suggest the presence of a counter-rotation in the obscuring torus of NGC
1068. We propose to explain this phenomenon as due to the influence of a wind,
considered as radiation pressure, and the effects of torus orientation. In
order to test this idea: 1. we make $N$-body simulation of a clumpy torus
taking into account mutual forces between particles (clouds); 2. we apply
ray-tracing algorithm with the beams from the central engine to choose the
clouds in the torus throat that can be under direct influence of the accretion
disk emission; 3. we use semi-analytical model to simulate the influence of the
asymmetrical radiation pressure (wind) forced on the clouds in the torus
throat. An axis of such a wind is tilted with respect to the torus symmetry
axis; 4. we orient the torus relative to an observer and again apply
ray-tracing algorithm. In this step the beams go from an observer to the
optically thick clouds that allows us to take into account the mutual
obscuration of clouds; 5. after projecting on the picture plane, we impose a
grid on the resulting cloud distribution and find the mean velocity of clouds
in each cells to mimic the ALMA observational maps. By choosing the parameters
corresponding to NGC 1068 we obtain the model velocity maps that emulate the
effect of an apparent counter-rotation and can explain the discovery made by
ALMA.
