Analysis of the Helical Kink Stability of Differently Twisted Magnetic Flux Ropes

• Published in: Solar physics Vol. 295; no. 9
• Main Authors: Florido-Llinas, M., Nieves-Chinchilla, T., Linton, M. G.
• Format: Journal Article
• Language: English
• Published: Dordrecht Springer Netherlands 01.09.2020; Springer Nature B.V
• Subjects: Astrophysics and Astroparticles; Atmospheric Sciences; Chirality; Coronal mass ejection; Editors’ Choice; Fluctuations; Geomagnetic activity; Geomagnetism; Helicity; Heliosphere; Laboratories; Magnetic fields; Magnetic flux; Magnetic structure; Magnetism; Numerical methods; Physics; Physics and Astronomy; Plasma; Solar Orbiter (ESA); Solar orbits; Solar physics; Solar probes; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Stability analysis; Towards Future Research on Space Weather Drivers; Coronal mass ejections; Flux ropes; Twist distribution; Kink instability; Magnetic fields
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/s11207-020-01687-z

Magnetic flux ropes (MFRs) are usually considered to be the magnetic structure that dominates the transport of helicity from the Sun into the heliosphere. They entrain a confined plasma within a helically organized magnetic structure and are able to cause geomagnetic activity. The formation, evolution, and twist distribution of MFRs are issues subject to strong debate. Although different twist profiles have been suggested so far, none of them has been thoroughly explored yet. The aim of this work is to present a theoretical study of the conditions under which MFRs with different twist profiles are kink stable and thereby shed some light on the aforementioned aspects. The magnetic field is modeled according to the circular–cylindrical analytical flux rope model in Nieves-Chinchilla et al. ( Astrophys. J. 823 , 27, 2016 ) as well as the Lundquist and Gold–Hoyle models, and the kink stability is analyzed with a numerical method that has been developed based on Linton, Longcope, and Fisher ( Astrophys. J. 469 , 954, 1996 ). The results are discussed in relation to MFR rotations, magnetic forces, the reversed chirality scenario, and the expansion throughout the heliosphere, among others, providing a theoretical background to improve the current understanding of the internal magnetic configuration of coronal mass ejections (CMEs). The data obtained by new missions like Parker Solar Probe or Solar Orbiter will give the opportunity to explore these results and ideas by observing MFRs closer than ever to the Sun.