Super Eddington Slim Accretion Disks with Winds

TL;DR

This paper models super-Eddington slim accretion disks around black holes, incorporating porous layers to reduce opacity, revealing that such disks can remain slim and produce powerful winds even at super-Eddington accretion rates.

Contribution

It introduces a new model of super-Eddington slim disks with porous layers, showing they can sustain high accretion rates and drive winds without becoming geometrically thick.

Findings

Disks remain slim at high accretion rates despite radiation pressure dominance.

Net luminosity exceeds Eddington luminosity above 1.5 times the critical rate.

Winds become spherical at very high accretion rates, limiting the model.

Abstract

We construct Super-Eddington Slim Disks models around both stellar and super-massive black holes by allowing the formation of a porous layer with a reduced effective opacity. We show that at high accretion rates, the inner part of the disks become radiation pressure dominated. However, unlike the standard scenario in which the disks become thick, super-Eddington disks remain slim. In addition, they accelerate a significant wind with a "thick disk" geometry. We show that above about 1.5 times the standard critical mass accretion rate (needed to release the Eddington luminosity), the net luminosity released is above Eddington. At above about 5 times the standard critical rate, the central BH accretes more than the Eddington accretion rate. Above about 20 m-dot_crit, the disk remains slim but the wind becomes spherical, and the present model breaks down.