# Episodic Jets from Black Hole Accretion Disks

## TL;DR

This paper proposes a model where relativistic plasmoids ejected from black hole accretion disks are driven by toroidal instability, successfully explaining observed jet phenomena in active galactic nuclei and microquasars.

## Contribution

It introduces a novel application of toroidal instability to explain episodic jet ejections from black hole accretion disks, linking plasma physics with astrophysical observations.

## Key findings

- Model predictions align with observed plasmoid trajectories in 3C120.
- The mechanism explains the timing of jet ejections following X-ray dips.
- The approach bridges laboratory plasma physics and astrophysical jet phenomena.

## Abstract

Several active galactic nuclei and microquasars are observed to eject plasmoids that move at relativistic speeds. We envisage the plasmoids as pre-existing current carrying magnetic flux ropes that were initially anchored in the accretion disk-corona. The plasmoids are ejected outwards via a mechanism called the toroidal instability (TI). The TI, which was originally explored in the context of laboratory tokamak plasmas, has been very successful in explaining coronal mass ejections from the Sun. Our model predictions for plasmoid trajectories compare favorably with a representative set of multi-epoch observations of radio emitting knots from the radio galaxy 3C120, which were preceded by dips in Xray intensity.