Jets from accretion disk dynamos: consistent quenching modes for dynamo and resistivity

TL;DR

This study uses non-ideal MHD simulations to explore how magnetic fields generated by dynamos influence jet launching from accretion disks, emphasizing consistent quenching modes and their effects on jet properties.

Contribution

It introduces a more consistent mean-field dynamo model incorporating magnetic quenching of turbulence and diffusivity, analyzing its impact on disk magnetization and jet characteristics.

Findings

Stronger dynamo quenching saturates magnetic fields at lower disk magnetization.

Jet properties remain consistent across different dynamo feedback models.

Magnetic field reversals and intermittent flaring are linked to flux rope dynamics and reconnection.

Abstract

Astrophysical jets are launched from strongly magnetized systems that host an accretion disk surrounding a central object. The origin of the magnetic field, which is a key component of the launching process, is still an open question. Here we address the question of how the magnetic field required for jet launching is generated and maintained by a dynamo process. By carrying out non-ideal MHD simulations (PLUTO code), we investigate how the feedback of the generated magnetic field on the mean-field dynamo affects the disk and jet properties. We find that a stronger quenching of the dynamo leads to a saturation of the magnetic field at a lower disk magnetization. Nevertheless, we find that, while applying different dynamo feedback models, the overall jet properties remain unaffected. We then investigate a feedback model which encompasses a quenching of the magnetic diffusivity. Our modeling considers a more consistent approach for mean-field dynamo modeling simulations, as the magnetic quenching of turbulence should be considered for both, a turbulent dynamo and turbulent magnetic diffusivity. We find that, after the magnetic field is saturated, the Blandford-Payne mechanism can work efficiently, leading to more collimated jets, that move, however, with slower speed. We find strong intermittent periods of flaring and knot ejection for low Coriolis numbers. In particular, flux ropes are built up and advected towards the inner disk thereby cutting off of the inner disk wind, leading to magnetic field reversals, reconnection and the emergence of intermittent flares.