  Outflows produced by a supermassive black hole (SMBH) can have important
feedback effects in its host galaxy. An unresolved question is the nature and
properties of winds from SMBHs accreting at low rates in low-luminosity active
galactic nuclei (LLAGNs). We performed two-dimensional numerical,
hydrodynamical simulations of radiatively inefficient accretion flows onto non
spinning black holes. We explored a diversity of initial conditions in terms of
rotation curves and viscous shear stress prescriptions, and evolved our models
for very long durations of up to $8 \times 10^5 GM/c^3$. Our models resulted in
powerful subrelativistic, thermally-driven winds originated from the corona of
the accretion flow at distances $10-100 GM/c^2$ from the SMBH. The winds
reached velocities of up to $0.01 c$ with kinetic powers corresponding to
0.1-1% of the rest-mass energy associated with inflowing gas at large
distances, in good agreement with models of the "radio mode" of AGN feedback.
The properties of our simulated outflows are in broad agreement with
observations of winds in quiescent galaxies that host LLAGNs, which are capable
of heating ambient gas and suppressing star formation.
