Magnetohydrodynamic numerical simulation of the outflows driven by magnetic field and radiation force from the corona above a thin disk. (arXiv:1906.07364v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yang_X/0/1/0/all/0/1">Xiao-Hong Yang</a> (CQU), <a href="http://arxiv.org/find/astro-ph/1/au:+Bu_D/0/1/0/all/0/1">De-Fu Bu</a> (SHAO), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Q/0/1/0/all/0/1">Qi-Xiu Li</a> (CQU)
A hot corona is suggested to be above the standard thin disk. The anisotropy
of hard X-ray emission in radio-quiet active galactic nuclei implies that the
corona is not static and probably moves outwards like winds. We perform
two-dimensional magnetohydrodynamical simulations to study the outflowing
corona driven by magnetic field and radiation force. In our simulations, as the
initial state and the boundary condition at the disk surface, the corona
temperature is set to $10^9$ K inside 10 Schwarzschild radius ($r_{rm s}$)
while the corona temperature is set to $10^7$ K outside 10 $r_{rm s}$. We
employ a weak poloidal magnetic field as the initial magnetic field. A
collimated outflow and a wide-angle ordered outflow are observed in our
simulations. The collimated outflow is around the rotational axis and has a
bulk velocity of $sim$0.03–0.3 $c$ ( $c$ is speed of light) at 90 $r_{rm
s}$, while their mass outflow rate is very low. The collimated outflow is a
weak jet. The wide-angle ordered outflow is distributed at the middle and high
latitude and moves outwards with a velocity of $10^2$–$10^4$ Km s$^{-1}$. The
outflow velocity depends on the disk luminosity. The gas around the disk
surface is turbulent, especially outside 10 $r_{rm s}$. The other properties
of outflows are discussed in details.
A hot corona is suggested to be above the standard thin disk. The anisotropy
of hard X-ray emission in radio-quiet active galactic nuclei implies that the
corona is not static and probably moves outwards like winds. We perform
two-dimensional magnetohydrodynamical simulations to study the outflowing
corona driven by magnetic field and radiation force. In our simulations, as the
initial state and the boundary condition at the disk surface, the corona
temperature is set to $10^9$ K inside 10 Schwarzschild radius ($r_{rm s}$)
while the corona temperature is set to $10^7$ K outside 10 $r_{rm s}$. We
employ a weak poloidal magnetic field as the initial magnetic field. A
collimated outflow and a wide-angle ordered outflow are observed in our
simulations. The collimated outflow is around the rotational axis and has a
bulk velocity of $sim$0.03–0.3 $c$ ( $c$ is speed of light) at 90 $r_{rm
s}$, while their mass outflow rate is very low. The collimated outflow is a
weak jet. The wide-angle ordered outflow is distributed at the middle and high
latitude and moves outwards with a velocity of $10^2$–$10^4$ Km s$^{-1}$. The
outflow velocity depends on the disk luminosity. The gas around the disk
surface is turbulent, especially outside 10 $r_{rm s}$. The other properties
of outflows are discussed in details.
http://arxiv.org/icons/sfx.gif
