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We report on a new class of solutions of black hole accretion disks that wehave found through three-dimensional, global, radiative magnetohydrodynamicsimulations in general relativity.  It combines features of the canonical thin, slim and thick disk models butdiffers in crucial respects from each of them. We expect these new solutions toprovide a more realistic description of black hole disks than the slim diskmodel. We are presenting a disk solution for a non-spinning black hole at asub-Eddington mass accretion rate, $\dot M=0.6\,\dot M_{\rm Edd}$. By thedensity scale-height measure the disk appears to be thin, having a high densitycore near the equatorial plane of height $h_{\rho} \sim 0.1 \,r$, but most ofthe inflow occurs through a highly advective, turbulent, optically thick,Keplerian region that sandwiches the core and has a substantial geometricalthickness comparable to the radius, $H \sim r$. The accreting fluid issupported above the midplane in large part by the magnetic field, with the gasand radiation to magnetic pressure ratio $\beta \sim 1$, this makes the diskthermally stable, even though the radiation pressure strongly dominates overgas pressure. A significant part of the radiation emerging from the disk iscaptured by the black hole, so the disk is less luminous than a thin disk wouldbe at the same accretion rate.

Puffy accretion disks: sub-Eddington, optically thick, and stable