The properties of wind and jet from a super-Eddington accretion flow around a supermassive black hole

TL;DR

This study uses radiation magnetohydrodynamical simulations to analyze wind and jet properties from a super-Eddington accretion flow around a supermassive black hole, revealing wind's dominant role in AGN feedback.

Contribution

It provides detailed measurements of wind and jet fluxes using a novel virtual particle trajectory method in super-Eddington accretion flows, highlighting wind's importance.

Findings

Wind mass flux is 2-6 times higher than previous estimates.

Wind's momentum flux exceeds that of jet.

Jet's total energy flux is up to 3 times that of wind.

Abstract

Wind and jet are important medium of AGN feedback thus it is crucial to obtain their properties for the feedback study. In this paper we investigate the properties of wind and jet launched from a magnetized super-Eddington accretion flow around a supermassive black hole. For this aim, we have performed radiation magnetohydrodynamical simulation of a magnetically arrested super-Eddington accretion flows. We then have analyzed the simulation data by the ``virtual particle trajectory'' approach and obtained the mass flux, poloidal and toroidal velocities, and mass-flux-weighted momentum and energy fluxes of wind and jet. The mass flux is found to be 2-6 times higher than that obtained based on the time-averaged streamline method widely used in literature. The momentum flux of wind is found to be larger than that of jet, while the total energy flux of jet is at most 3 times larger than that of wind. These results are similar to the case of hot accretion flows and imply that winds likely play a more important role than jet in AGN feedback. The acceleration mechanism of wind and jet is analyzed and found to be dominated by Lorentz force rather than radiation force.