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

Florido-Llinas, M.; Nieves‐Chinchilla, Teresa; Linton, M. G.

doi:10.1007/s11207-020-01687-z

Cited by 15 publications

(19 citation statements)

References 80 publications

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“…Since we assume a constant τ of 1, we expect the flux rope to become kink unstable for a C below 1.7 according to Florido‐Llinas et al. (2020). The force‐free and drag‐only cases initially begin increasing.…”

Section: Ensemble Study Resultsmentioning

confidence: 99%

“…The middle panel shows the change in C, which scales the poloidal field relative to B 0 and evolves based on the relative size and shape of the CME. Since we assume a constant τ of 1, we expect the flux rope to become kink unstable for a C below 1.7 according to Florido-Llinas et al (2020). The force-free and drag-only cases initially begin increasing.…”

Section: Cme Magnetic Fieldmentioning

confidence: 99%

“…Florido‐Llinas et al. (2020) find that only certain combinations of C and τ are stable with respect to the kink instability. ANTEATR‐PARADE does not calculate any torques that could alter the orientation of the flux rope so approaching an unstable combination of C and τ will not produce any kinking.…”

Section: Anteatr‐parade Modelmentioning

confidence: 99%

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Modeling Interplanetary Expansion and Deformation of CMEs With ANTEATR‐PARADE: Relative Contribution of Different Forces

Kay

Nieves‐Chinchilla

2021

JGR Space Physics

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Understanding the interplanetary behavior of CMEs is critical for accurate space weather forecasting. The severity of a geomagnetic storm depends on the CME properties at the time of impact, mostly significantly the magnetic field but also its size and kinematic properties. Accordingly, we must not only understand the properties with which a CME is initiated, but how they evolve during its propagation if we wish to know the severity and timing of an impact (e.g., Manchester et al., 2017). Kilpua et al. (2019) provides an in depth summary on many of the challenges of forecasting CMEs.We tend to have an abundance of coronal images from the Earth's perspective, both in visible light and the extreme ultraviolet, which have allowed us to study the source region and early evolution of Earth-impacting CMEs for nearly half of a century (e.g., Tousey, 1973), but routine observations from off the Sun-Earth line are limited to the coronagraphs or heliospheric imagers on the STEREO satellites. Parker Solar Probe

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Section: Ensemble Study Resultsmentioning

confidence: 99%

Section: Cme Magnetic Fieldmentioning

confidence: 99%

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Modeling Interplanetary Expansion and Deformation of CMEs With ANTEATR‐PARADE: Relative Contribution of Different Forces

Kay

Nieves‐Chinchilla

2021

JGR Space Physics

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“…Observations also suggest that the CME, and presumably the MFR, undergo significant evolutionary changes, such as rotation, deformation, or distortion during their heliospheric propagation, among others, (Burlaga et al 2002;Nieves-Chinchilla et al 2012;Manchester et al 2017;Florido-Llinas et al 2020), with a small number of ICMEs evolving in the shape of outwardconcave arcs (Kahler & Webb 2007). To better understand the effects of the evolutionary processes in the CME, the in-situ measurements are compared with the remote-sensing observations.…”

Section: Introductionmentioning

confidence: 99%

Evidence of a complex structure within the 2013 August 19 coronal mass ejection. Radial and longitudinal evolution in the inner heliosphere

Rodríguez-García,

Nieves-Chinchilla,

Gómez-Herrero

et al. 2022

Preprint

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Context. Late on 2013 August 19, a coronal mass ejection (CME) erupted from an active region located near the far-side central meridian from Earth's perspective. The event and its accompanying shock were remotely observed by the STEREO-A, STEREO-B and SOHO spacecraft. The interplanetary counterpart (ICME) was intercepted by MESSENGER near 0.3 au, and by both STEREO-A and STEREO-B, near 1 au, which were separated by 78 • in heliolongitude. Aims. The main objective of this study is to follow the radial and longitudinal evolution of the ICME throughout the inner heliosphere, and to examine possible scenarios for the different magnetic flux-rope configuration observed on the solar disk, and measured in situ at the locations of MESSENGER and STEREO-A, separated by 15 • in heliolongitude, and at STEREO-B, which detected the ICME flank. Methods. Solar disk observations are used to estimate the 'magnetic flux-rope type', namely, the magnetic helicity, axis orientation and axial magnetic field direction of the flux rope. The graduated cylindrical shell model is used to reconstruct the CME in the corona. The analysis of in-situ data, specifically, plasma and magnetic field, is used to estimate the global interplanetary shock geometry and to derive the magnetic flux-rope type at different in-situ locations, which is compared to the type estimated from solar disk observations. The elliptical cylindrical analytical model is used for the in-situ magnetic flux-rope reconstruction. Results. Based on the CME geometry and on the spacecraft configuration, we find that the magnetic flux-rope structure detected at STEREO-B belongs to the same ICME detected at MESSENGER and STEREO-A. The opposite helicity deduced at STEREO-B, might be due to the spacecraft intercepting one of the legs of the structure far from the flux-rope axis, while STEREO-A and MESSENGER are crossing through the core of the magnetic flux rope. The different flux-rope orientations measured at MESSENGER and STEREO-A arise probably because the two spacecraft measure a curved, highly distorted and rather complex magnetic flux-rope topology. The ICME may have suffered additional distortion in its evolution in the inner heliosphere, such as the west flank is propagating faster than the east flank when arriving near 1 au. Conclusions. This work illustrates how a wide, curved, highly distorted and rather complex CME was showing different orientations as observed on the solar disk and measured in situ at 0.3 au and near 1 au. It shows how the ambient conditions can significantly affect the expansion and propagation of the CME/ICME, introducing additional irregularities to the already asymmetric eruption. The study also manifests how these complex structures cannot be directly reconstructed with the current models available, and that multi-point analysis is of the utmost importance in such complex events.

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“…CME evolution and propagation in the heliosphere is still one of the critical areas of research. In this collection, there are several studies that span from a case event analysis, data analysis, 3D simulation, theoretical understanding of the physical processes associated with the evolution, and identification of the internal structure based on artificial intelligence techniques (Davies et al, 2020;Balmaceda et al, 2020;Desai et al, 2020;Florido-Llinas, Nieves-Chinchilla, and Linton, 2020;dos Santos et al, 2020). As stated by Balmaceda et al (2020) (Editor's choice), a proper characterization of the kinematics of CMEs is important not only for practical purposes, i.e.…”

mentioning

confidence: 99%

Editorial: Towards Future Research on Space Weather Drivers

2021

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

Cited by 15 publications

References 80 publications

Modeling Interplanetary Expansion and Deformation of CMEs With ANTEATR‐PARADE: Relative Contribution of Different Forces

Modeling Interplanetary Expansion and Deformation of CMEs With ANTEATR‐PARADE: Relative Contribution of Different Forces

Evidence of a complex structure within the 2013 August 19 coronal mass ejection. Radial and longitudinal evolution in the inner heliosphere

Editorial: Towards Future Research on Space Weather Drivers

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