A Breakout Model for Solar Coronal Jets with Filaments

TL;DR

This paper presents 3D MHD simulations of solar coronal jets involving mini-filaments, extending the magnetic-breakout model to explain various observed features of these small-scale eruptions.

Contribution

It introduces a detailed 3D MHD simulation study of mini-filament jets, applying the magnetic-breakout mechanism to small-scale solar eruptions.

Findings

Breakout-jet mechanism is robust across different simulations.

Different model realizations explain various observational features.

Mini-filament eruptions follow the magnetic-breakout process.

Abstract

Recent observations have revealed that many solar coronal jets involve the eruption of miniature versions of large-scale filaments. Such "mini-filaments" are observed to form along the polarity inversion lines of strong, magnetically bipolar regions embedded in open (or distantly closing) unipolar field. During the generation of the jet, the filament becomes unstable and erupts. Recently we described a model for these mini-filament jets, in which the well-known magnetic-breakout mechanism for large-scale coronal mass ejections is extended to these smaller events. In this work we use three-dimensional magnetohydrodynamic simulations to study in detail three realisations of the model. We show that the breakout-jet generation mechanism is robust and that different realisations of the model can explain different observational features. The results are discussed in relation to recent observations and previous jet models.