Using two-dimensional simulations of non-radiative viscous rotating black hole accretion flows , we show that the flows with \alpha \sim 0.1 - 0.3 self-organize to form stationary unipolar or bipolar outflows accompanied by global meridional circulations .
The required energy comes , with efficiency \sim 0.001 - 0.01 , from the matter directly accreted onto black hole .
Observational implications are discussed .