Puffy accretion disk is model of a stable accretion disk obtained purely via a general relativistic radiative magnetohydrodynamical simulation. It combines features of the thin, slim, and thick disk models but differs in crucial respects from each of them. We expect the new solution to provide a more realistic description of black hole disks than the slim disk model. We are presenting a disk solution for a nonspinning black hole at a sub-Eddington mass accretion rate. Although the density scale-height of the disk appears to be thin with a high density core near the equatorial plane, most of the inflow occurs through a highly advective, turbulent, optically thick, Keplerian region surrounding the core. Stability of the solution is supported in large part by the magnetic field, even though the radiation pressure strongly dominates over gas pressure.