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.

中文翻译：

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异捻磁通绳螺旋扭结稳定性分析

磁通量绳（MFR）通常被认为是主导从太阳到日光层的螺旋度传输的磁性结构。它们在螺旋状组织的磁结构中夹带受限等离子体，并能够引起地磁活动。MFR 的形成、演化和扭曲分布是备受争议的问题。尽管到目前为止已经提出了不同的扭曲曲线，但还没有对它们进行彻底的探索。这项工作的目的是对具有不同扭曲曲线的 MFR 扭结稳定的条件进行理论研究，从而对上述方面有所了解。磁场是根据 Nieves-Chinchilla 等人的圆柱分析磁通绳模型建模的。（天体物理学。J. 823, 27, 2016) 以及 Lundquist 和 Gold-Hoyle 模型，并使用基于 Linton、Longcope 和 Fisher (Astrophys. J. 469, 954, 1996) 开发的数值方法分析扭结稳定性。讨论了与 MFR 旋转、磁力、反向手性情景和整个日光层的扩张等相关的结果，为提高目前对日冕物质抛射 (CME) 的内部磁构型的理解提供了理论背景。帕克太阳探测器或太阳轨道器等新任务获得的数据将有机会通过观察比以往更接近太阳的 MFR 来探索这些结果和想法。954, 1996)。讨论了与 MFR 旋转、磁力、反向手性情景和整个日光层的扩张等相关的结果，为提高目前对日冕物质抛射 (CME) 的内部磁构型的理解提供了理论背景。帕克太阳探测器或太阳轨道器等新任务获得的数据将有机会通过观察比以往更接近太阳的 MFR 来探索这些结果和想法。954, 1996)。讨论了与 MFR 旋转、磁力、反向手性情景和整个日光层的扩张等相关的结果，为提高目前对日冕物质抛射 (CME) 的内部磁构型的理解提供了理论背景。帕克太阳探测器或太阳轨道器等新任务获得的数据将有机会通过观察比以往更接近太阳的 MFR 来探索这些结果和想法。