The Ubiquity of Twisted Flux Ropes in the Quiet Sun

TL;DR

This paper demonstrates that twisted flux ropes are widespread in the quiet Sun, contain enough energy to cause eruptions, and are driven by a small-scale dynamo, contributing to atmospheric heating and magnetic activity.

Contribution

It provides high-resolution observations and simulations showing the ubiquity and energetic role of TFRs in the quiet Sun, linking them to small-scale dynamo processes.

Findings

TFRs are associated with mesospots and large-scale magnetic fields.

They contain sufficient free magnetic energy to trigger eruptions.

TFRs are generated by a small-scale dynamo process.

Abstract

Models and observations have demonstrated that Twisted Flux Ropes (TFRs) play a significant role in the structure and eruptive dynamics of active regions. Their role in the dynamics of the quiet Sun atmosphere on has remained elusive, their fundamental relevance emerging mainly from theoretical models (Amari et al. 2015), showing that they form and erupt as a result of flux cancellation. Here HINODE high-resolution photospheric vector magnetic field measurements are integrated with advanced environment reconstruction models: TFRs develop on various scales and are associated with the appearance of mesospots. The developing TFRs contain sufficient free magnetic energy to match the requirements of the recently observed "campfires" discovered by Solar Orbiter in the quiet Sun. The free magnetic energy is found to be large enough to trigger eruptions while the magnetic twist large enough to trigger confined eruptions, heating the atmosphere. TFRs are also connected to larger scale magnetic fields such as supergranulation loops, allowing the generation of Alfv\'en waves at the top of the chromosphere that can propagate along them. High-resolution magnetohydrodynamic simulations, incorporating subsurface dynamo activity at an unprecedented 30 km spatial resolution, confirm that TFRs are ubiquitous products of the permanent small scale dynamo engine that feeds their formation, destabilization, eruption via flux emergence, submergence and cancellation of their chromospheric feet, similar to the dynamics driving large scale eruptive events. Future investigations, especially with the Daniel K. Inouye Solar Telescope (DKIST) and Solar Orbiter will deepen our understanding of TFRs in the context of atmospheric heating.