Modelling MHD accretion-ejection - episodic ejections of jets triggered by a mean-field disk dynamo

TL;DR

This paper uses MHD simulations with a mean-field dynamo to study episodic jet ejections from accretion disks, revealing how magnetic field generation and suppression influence jet activity and structure.

Contribution

It introduces a self-consistent mean-field dynamo model that explains episodic jet ejections and large-scale jet knots in accretion disks.

Findings

Dynamo-driven magnetic fields enable episodic jet ejections.

Suppression of the dynamo inhibits outflow and accretion.

Outer disk fields are highly inclined and influence jet collimation.

Abstract

We present MHD simulations exploring the launching, acceleration and collimation of jets and disk winds. The evolution of the disk structure is consistently taken into account. Extending our earlier studies, we now consider the self-generation of the magnetic field by an $\alpha^2\Omega$ mean-field dynamo. The disk magnetization remains on a rather low level, that helps to evolve the simulations for $T > 10,000$ dynamical time steps on a domain extending 1500 inner disk radii. We find a magnetic field of the inner disk similar to the commonly found open field structure, favoring magneto-centrifugal launching. The outer disk field is highly inclined and predominantly radial. Here, differential rotation induces a strong toroidal component that plays a key role in outflow launching. These outflows from the outer disk are slower, denser, and less collimated. If the dynamo action is not quenched, magnetic flux is continuously generated, diffuses outward the disk, and fills the entire disk. We have invented a toy model triggering a time-dependent mean-field dynamo. The duty cycles of this dynamo lead to episodic ejections on similar timescales. When the dynamo is suppressed as the magnetization falls below a critical value, the generation of the outflows and also accretion is inhibited. The general result is that we can steer episodic ejection and {\em large-scale jet knots} by a {\em disk-intrinsic dynamo} that is time-dependent and regenerates the jet-launching magnetic field.