The Emergence of a Twisted Flux Tube into the Solar Atmosphere: Sunspot Rotations and the Formation of a Coronal Flux Rope
Y. Fan

TL;DR
This paper uses 3D simulations to show how twisted magnetic flux tubes emerge from the solar interior, induce sunspot rotations, and form coronal flux ropes that can lead to solar eruptions.
Contribution
It demonstrates the process of flux emergence, sunspot rotation, and flux rope formation through nonlinear torsional Alfvén waves in a detailed 3D simulation.
Findings
Rotational motions twist the magnetic field into an inverse configuration.
A sigmoid-shaped flux rope forms in the corona with increasing twist.
Flux ropes develop significant magnetic energy, potentially leading to eruptions.
Abstract
We present a 3D simulation of the dynamic emergence of a twisted magnetic flux tube from the top layer of the solar convection zone into the solar atmosphere and corona. It is found that after a brief initial stage of flux emergence during which the two polarities of the bipolar region become separated and the tubes intersecting the photosphere become vertical, significant rotational motion sets in within each polarity. The rotational motions of the two polarities are found to twist up the inner field lines of the emerged fields such that they change their orientation into an inverse configuration (i.e. pointing from the negative polarity to the positive polarity over the neutral line). As a result, a flux rope with sigmoid-shaped, dipped core fields form in the corona, and the center of the flux rope rises in the corona with increasing velocity as the twisting of the flux rope…
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