Speaker
Description
Accretion flows that transfer gas at rates exceeding the Eddington limit
are optically thick but exhibit lower radiative efficiency compared to
thin discs. In this study, we present Radiative General Relativistic
Magnetohydrodynamic (GRRMHD) simulations of (intermediate)
super-Eddington accretion onto a black hole with a mass of 10 solar
masses, modeling ultra-luminous X-ray sources. Our simulations show
significant gas outflows and radiative winds escaping from the polar
region. We analyze the inner density and temperature structure and the
decomposition the total energy flux into various components (e.g.,
thermal, magnetic/viscous, and radiative), illustrating how accretion
processes convert the stored gravitational binding energy into
radiation. Finally, we provide a rough estimation of the apparent
isotropic luminosity, which is highly collimated along the polar axis.
