Kink instability of flux ropes in partially-ionised plasmas

TL;DR

This paper investigates how partial ionisation influences the kink instability in solar flux ropes, revealing faster development and more energetic eruptions, which are key to understanding chromospheric heating and jet formation.

Contribution

It provides the first detailed analysis of kink instability development in partially-ionised plasmas, highlighting the effects of charge-neutral interactions on instability growth and energy release.

Findings

Partial ionisation accelerates the kink instability onset.

Increased internal energy and faster temperature rise in PIP cases.

More explosive flux rope dynamics in partially-ionised plasmas.

Abstract

In the solar atmosphere, flux ropes are subject to current driven instabilities that are crucial in driving plasma eruptions, ejections and heating. A typical ideal magnetohydrodynamics (MHD) instability developing in flux ropes is the helical kink, which twists the flux rope axis. The growth of this instability can trigger magnetic reconnection, which can explain the formation of chromospheric jets and spicules, but its development has never been investigated in a partially-ionised plasma (PIP). Here we study the kink instability in PIP to understand how it develops in the solar chromosphere, where it is affected by charge-neutral interactions. Partial ionisation speeds up the onset of the non-linear phase of the instability, as the plasma $\beta$ of the isolated plasma is smaller than the total plasma $\beta$ of the bulk. The distribution of the released magnetic energy changes in fully and partially-ionised plasmas, with a larger increase of internal energy associated to the PIP cases. The temperature in PIP increases faster also due to heating terms from the two-fluid dynamics. PIP effects trigger the kink instability on shorter time scales, which is reflected in a more explosive chromospheric flux rope dynamics. These results are crucial to understand the dynamics of small-scale chromospheric structures - mini-filament eruptions - that this far have been largely neglected but could significantly contribute to chromospheric heating and jet formation.