The material accreting onto Sgr A* most probably comes from the nearby stars .
We analyze the pattern of this flow at distances of a fraction of a parsec and we argue that the net angular momentum of this material is low but non-negligible , and the initially supersonic disk accretion changes into subsonic flow with constant angular momentum .
Next we estimate the flow parameters at a distance R _ { BHL } from the black hole and we argue that for the plausible parameter range the accretion flow is non-stationary .
The inflow becomes supersonic at distance of \sim 10 ^ { 4 } R _ { g } but the solution does not continue below the horizon and the material piles up forming a torus , or a ring , at a distance of a few up to tens of Schwarzchild radii .
Such a torus is known to be unstable and may explain strong variability of the flow in Sgr A* .
Our considerations show that the temporary formation of such a torus seems to be unavoidable .
Our best fitting model predicts a rather large accretion rate of around 4 \cdot 10 ^ { -6 } M _ { \odot } / yr directly on Sgr A* .
We argue that magnetic fields in the flow are tangled and this allows our model to overcome the disagreement with the Faraday rotation limits .