Analysis of the Helical Kink Stability of Differently Twisted Magnetic Flux Ropes
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Analysis of the Helical Kink Stability of Differently Twisted Magnetic Flux Ropes M. Florido-Llinas1 M. G. Linton3
· T. Nieves-Chinchilla2
·
Received: 27 February 2020 / Accepted: 10 August 2020 © Springer Nature B.V. 2020
Abstract 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 This article belongs to the Topical Collection: Towards Future Research on Space Weather Drivers Guest Editors: Hebe Cremades and Teresa Nieves-Chinchilla
B M. Florido-Llinas
[email protected] T. Nieves-Chinchilla [email protected] M.G. Linton [email protected]
1
Interdisciplinary Higher Education Center (CFIS), Polytechnic University of Catalonia, Pau Gargallo 14, Barcelona 08028, Spain
2
Heliophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt MD 20771, USA
3
Naval Research Laboratory, 4555 Overlook Avenue SW, Washington, DC 20375, USA
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opportunity to explore these results and ideas by observing MFRs closer than ever to the Sun. Keywords Flux ropes · Twist distribution · Kink instability · Coronal mass ejections · Magnetic fields
1. Introduction Coronal mass ejections (CMEs) are large eruptions of magnetized plasma from the solar corona into the heliosphere and one of the main drivers of adverse space weather. They are able to severely impact telecommunications or space systems due to the injection of solar magnetic energy into the magnetosphere, which results from magnetic reconnection processes between the CME and the terrestrial magnetic field. Magnetic flux ropes (MFRs) are fundamental plasma structures that frequently appear in the heliosphere as part of CMEs. They
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