  We use global three dimensional radiation magneto-hydrodynamical simulations
to study accretion disks onto a $5\times 10^8M_{\odot}$ black hole with
accretion rates varying from $\sim 250L_{Edd}/c^2$ to $1500 L_{Edd}/c^2$. We
form the disks with torus centered at $50-80$ gravitational radii with
self-consistent turbulence initially generated by the magneto-rotational
instability. We study cases with and without net vertical magnetic flux. The
inner regions of all disks have radiation pressure $\sim 10^4-10^6$ times the
gas pressure. Non-axisymmetric density waves that steepen into spiral shocks
form as gas flows towards the black hole. In simulations without net vertical
magnetic flux, Reynolds stress generated by the spiral shocks are the dominant
mechanism to transfer angular momentum. Maxwell stress from MRI turbulence can
be larger than the Reynolds stress only when net vertical magnetic flux is
sufficiently large. Outflows are formed with speed $\sim 0.1-0.4c$. When the
accretion rate is smaller than $\sim 500 L_{Edd}/c^2$, outflows start around
$10$ gravitational radii and the radiative efficiency is $\sim 5\%-7\%$ with
both magnetic field configurations. With accretion rate reaching $1500
L_{Edd}/c^2$, most of the funnel region close to the rotation axis becomes
optically thick and the outflow only develops beyond $50$ gravitational radii.
The radiative efficiency is reduced to $1\%$. We always find the kinetic energy
luminosity associated with the outflow is only $\sim 15\%-30\%$ of the
radiative luminosity. The mass flux lost in the outflow is $\sim 15\%-50\%$ of
the net mass accretion rates. We discuss implications of our simulation results
on the observational properties of these disks.
