Numerical Simulation of Hot Accretion Flows (III): Revisiting wind properties using trajectory approach

Abstract

Previous MHD simulations have shown that wind must exist in black hole hot accretion flows. In this paper, we continue our study by investigating the detailed properties of wind, such as mass flux and poloidal speed, and the mechanism of wind production. For this aim, we make use of a three dimensional GRMHD simulation of hot accretion flows around a Schwarzschild black hole. The simulation is designed so that the magnetic flux is not accumulated significantly around the black hole. To distinguish real wind from turbulent outflows, we track the trajectories of the virtual Largrangian particles from simulation data. We find two types of real outflows, i.e., a quasi-relativistic jet close to the axis and a sub-relativistic wind subtending a much larger solid angle. Most of the wind originates from the surface layer of the accretion flow. The poloidal wind speed almost remains constant once they are produced, but the flux-weighted wind speed roughly follows $v_{\mathrm{p},\mathrm{wind}}(r)\approx 0.25v_k(r)$. The mass flux of jet is much lower but the speed is much higher, $v_{\mathrm{p},\mathrm{jet}}\sim (0.3-0.4)c$. Consequently, both the energy and momentum fluxes of the wind are much larger than those of the jet. We find that the wind is produced and accelerated primarily by the combination of centrifugal force and magnetic pressure gradient, while the jet is mainly accelerated by magnetic pressure gradient. Finally, we find that the wind production efficiency ${\epsilon }_{\mathrm{wind}}\equiv {\dot{E}}_{\mathrm{wind}}/{\dot{M}}_{\mathrm{BH}}{c}^2\sim 1/1000$, in good agreement with the value required from large-scale galaxy simulations with AGN feedback.

13 pages, 13 figures; submitted to ApJ

References in corpus (4)

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• Ultra-fast outflows in radio-loud active galactic nuclei
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• AGN feedback in an isolated elliptical galaxy: the effect of strong radiative feedback in the kinetic mode

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