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