We present a scenario for non-radiative accretion onto the supermassive black hole at the galactic center .
Conducting MHD simulations with 1400 ^ { 3 } grid zones that break the axial and reflection symmetries of earlier investigations and extend inward from the Bondi radius , we find a quasi-hydrostatic radial density profile \rho \propto r ^ { -0.72 } with superadiabatic gradient corresponding to an n \sim 0.72 polytrope .
Buoyancy generated by magnetic dissipation is resisted by the same fields so effectively that energy is advected inward : a state of magnetically-frustrated convection .
This scenario is consistent with observational constraints on energetics andouter boundary conditions .