Magnetic flux emergence and solar eruptions in partially ionized plasmas

TL;DR

This study uses 3D MHD simulations to explore how partial ionization influences magnetic flux emergence and eruptions in the Sun, revealing differences in structure, speed, and eruption height compared to fully ionized models.

Contribution

It provides new insights into the effects of partial ionization on magnetic flux emergence and solar eruptions, extending previous models with detailed 3D simulations.

Findings

Emerging magnetic fields form arch-like structures with less twist in PI simulations.

Eruptions occur faster and at different heights in PI versus FI simulations.

Part of the eruptive flux rope temporarily carries neutrals into the high atmosphere.

Abstract

We have performed 3D MHD simulations to study the effect of partial ionization in the process of magnetic flux emergence in the Sun. In fact, we continue previous work and we now focus: 1) on the emergence of the magnetic fields above the solar photosphere and 2) on the eruptive activity, which follows the emergence into the corona. We find that in the simulations with partial ionization (PI), the structure of the emerging field consists of arch-like fieldlines with very little twist since the axis of the initial rising field remains below the photosphere. The plasma inside the emerging volume is less dense and it is moving faster compared to the fully ionized (FI) simulation. In both cases, new flux ropes (FR) are formed due to reconnection between emerging fieldlines, and they eventually erupt in an ejective manner towards the outer solar atmosphere. We are witnessing three major eruptions in both simulations. At least for the first eruption, the formation of the eruptive FR occurs in the low atmosphere in the FI case and at coronal heights in the PI case. Also, in the first PI eruption, part of the eruptive FR carries neutrals in the high atmosphere, for a short period of time. Overall, the eruptions are relatively faster in the PI case, while a considerable amount of axial flux is found above the photosphere during the eruptions in both simulations.