Super-Eddington Accretion Disks around Supermassive black Holes

Understand

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.