Numerical simulations of winds driven by radiation force from the corona above a thin disk

Abstract

Observations show that winds can be driven from the innermost region (inside a 50 Schwarschild radius) of a thin disk. It is interesting to study the winds launched from the innermost region. A hot corona above the black hole (BH) thin disk is irradiated by the disk. We perform two-dimensional hydrodynamical simulations to study the winds driven by radiation force from the corona in the innermost regions. The hard X-ray spectrum from active galactic nuclei (AGNs) suggests that the corona temperature is about $10^9$ K, so that we mainly analyze the properties of winds (or outflows) from the $10^9$ K corona. The disk luminosity plays an important role in driving the outflows. The more luminous the disk, the stronger the outflows. Mass outflow rate (${\dot{M}}_{\mathrm{out}}$) at a 90 Schwarschild radius depends on disk luminosity, which can be described as ${\dot{M}}_{\mathrm{out}}\propto 10^{3.3\Gamma }$ ($\Gamma$ is the ratio of the disk luminosity to the Eddington luminosity). In the case of high luminosity (e.g. $\Gamma =0.75$), the supersonic outflows with maximum speed $1.0\times 10^4$ Km s${}^{-1}$ are launched at $\sim 17^o$ --$30^o$ and $\sim 50^o$ --$80^o$ away from the pole axis. The Bernoulli parameter keeps increasing with the outward propagation of outflows. The radiation force keeps accelerating the outflows when outflows move outward. Therefore, we can expect the outflows to escape from the BH gravity and go to the galactic scale. The interaction between outflows and interstellar medium may be an important AGN feedback process.

arXiv comment9 pages, 12 figures, accepted for publication in ApJ

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• A magnetic accretion disk-outflow model for changing look active galactic nuclei
• Super-Eddington mass growth of intermediate-mass black holes embedded in dusty circumnuclear disks
• A global solution to a slim accretion disk with radiation-driven outflows
• A supercritical accretion disk with radiation-driven outflows
• Shocks in radiatively driven time dependent, relativistic jets around black holes
• Magnetohydrodynamic Winds Driven by the Line Force from the Standard Thin Disk around Supermassive Black Holes. I. The Case of Weak Magnetic Field
• Simulations of radiation driven winds from Keplerian discs
• Magnetohydrodynamic numerical simulation of the outflows driven by magnetic field and radiation force from the corona above a thin disk
• The dynamical structure of the outflows driven by a large-scale magnetic field
• Radiatively driven, time dependent bipolar outflows
• Effect of plasma composition on magnetized outflows
• Effect of radiation drag on the line-force-driven winds