The outflow from accretion disk around the Black Hole
The accretion disks around Black Holes(BHs) are believed to drive high energy astrophysical phenomena , such as high-energy radiation, disk outflows, and jets of Active Galactic Nuclei and black hole binaries.
But, structure of the disks and mechanisms of driving outflow have poorly understood. Especially, super-Eddington accretion disks, of which luminosity exceeds the Eddington luminosity, is a hot debated issue.
If the super-Eddington disks are feasible, the ultra luminous X-ray sources are explained without assuming intermediate mass black holes.
By two-dimensional radiation-hydrodynamics (2D-RHD) simulations, super-Eddington accretion disks around BHs are successfully reproduced, implying that quasi-steady super-Eddington accretion is possible (Ohsuga et al. 2005).However, the computational domain of the simulations is restricted tobe 500 Rs (Schwarzschild radius).Thus, the behavior of outflows at the distant region (>500Rs) is not investigated.
The structure of the super-Eddington flows might change if the outflowing matter of >500Rs get back to the vicinity of the black hole.
In order to understand more realistic structure and dynamics of the super-Eddington flows, it is needed to reperform 2D-RHD simulations with much larger computational domain.
In this talk, I present the fundamental mechanisms of BH accretion disks and outflows,and also my research plan of master thesis.
Finding Brown Dwarfs in star formation region with subaru telescope