The Wind Dynamics of Super-Eddington Sources in FRADO

TL;DR

This study uses 2.5D simulations to explore how super-Eddington accretion disks around black holes drive outflows via radiation pressure on dust, revealing mass-dependent outflow behaviors and feedback effects.

Contribution

It demonstrates that super-Eddington accretion disks produce significant dust-driven outflows with mass-dependent characteristics, expanding understanding of feedback in extreme accreting black holes.

Findings

Outflows can exceed accretion rates for black holes over 10^8 M_sun.

Failed winds occur only at larger radii in high accretors.

Outflows imply strong mechanical feedback despite stationarity.

Abstract

We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from $10^7$ up to $10^9 M_{\odot}$. Such high accretion rates are characteristic for extreme sources. We show that for high accretors radiatively dust-driving mechanism based on FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate strongly depends on the black hole mass, and in optically-thick energy-driven solution can exceed the accretion rate for masses larger than $10^ 8 M_{\odot}$ but momentum-driven outflow does not exceed the accretion rate even for super-Eddington accretion, therefore not violating the adopted stationarity of the disk. However, even in this case the outflow from the disk implies a strong mechanical feedback.