The super-critical accretion disk and outflow; an origin of the etc.

[Speaker 1]
Shino Nagisa
D2, SOKENDAI, Mitaka(supervisor : Mareki Honma)

[Speaker 2]
Katsuya Hashizume
D1, SOKENDAI, Mitaka(supervisor : Ken Ohsuga)
The super-critical accretion disk and outflow; an origin of the
ULX nebula
The accretion disks around black holes (BHs) are believed to drive
high energy astrophysical phenomena, such as high-energy radiation,
disk winds, and jets of active galactic nuclei and black hole
binaries. However, a central engine of ultra-luminous X-ray sources
(ULXs) is still an enigma. Since the luminosity of the ULXs exceeds
the Eddington luminosity of stellar mass BH (~10M_sun), the standard
disk (sub-Eddington disk) around the black hole of ~< 10Msun cannot explain the ULXs. Hence, two possibilities are suggested; (1) stellar mass BH with super-critical accretion disk of which the luminosity is larger than Eddington luminosity (2) standard disk around intermediate mass BH (IMBH) of > 100Msun.
Recently, multi-wavelength observations revealed that some of ULXs are
surrounded by nebulae (ULX nebulae). The origin of the nebulae has not
been understood yet, though it might be a key phenomenon to resolve
the central engine of the ULXs. Here, we investigate super-critical
accretion disk around stellar mass BH by two-dimensional
radiation-hydrodynamics simulations. We confirmed that super-critical
accretion disk drives strong outflows with large opening-angle (20-85
degree). The kinetic energy of the outflows is roughly consistent with
the luminosity injected into ULX nebulae, implying that our results
support the scenario of the stellar mass BHs with super-critical
accretion disks.