Evolution of a Magnetic Flux Rope toward Eruption

Wang, Wensi; Zhu, Chunming; Qiu, Jiong; Liu, Rui; Yang, Kai; Hu, Qiang

doi:10.3847/1538-4357/aaf3ba

Cited by 32 publications

(60 citation statements)

References 94 publications

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“…The CME was also observed by the twin Solar Terrestrial Relations Observatory (STEREO; Kaiser et al 2008) spacecraft orbiting the Sun close to 1 AU and, at the time of this study, separated from Earth by 116 • and 117 • , respectively. The onset and eruption of the 14 June 2012 CME from multi-wavelength imagery of the solar disc have been analysed extensively in several studies Palmerio et al 2017;Wang et al 2019). The first observation of the CME in white-light coronagraph images was at 13:25 UT in the STEREO's inner coronagraph COR1, which is part of the Sun Earth Connection Coronal and Heliospheric Investigation (SEC-CHI; Howard et al 2008) The NRH radio data 1 were processed using the standard So-larSoft NRH package to produce calibrated radio images of the Sun.…”

Section: Observations and Data Analysismentioning

confidence: 99%

Three-dimensional reconstruction of multiple particle acceleration regions during a coronal mass ejection

Morosan

Palmerio

Pomoell

et al. 2020

A&A

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Context. Some of the most prominent sources for particle acceleration in our Solar System are large eruptions of magnetised plasma from the Sun called coronal mass ejections (CMEs). These accelerated particles can generate radio emission through various mechanisms. Aims. CMEs are often accompanied by a variety of solar radio bursts with different shapes and characteristics in dynamic spectra. Radio bursts directly associated with CMEs often show movement in the direction of CME expansion. Here, we aim to determine the emission mechanism of multiple moving radio bursts that accompanied a flare and CME that took place on 14 June 2012. Methods. We used radio imaging from the Nançay Radioheliograph, combined with observations from the Solar Dynamics Observatory and Solar Terrestrial Relations Observatory spacecraft, to analyse these moving radio bursts in order to determine their emission mechanism and three-dimensional (3D) location with respect to the expanding CME. Results. In using a 3D representation of the particle acceleration locations in relation to the overlying coronal magnetic field and the CME propagation, for the first time, we provide evidence that these moving radio bursts originate near the CME flanks and some that are possible signatures of shock-accelerated electrons following the fast CME expansion in the low corona. Conclusions. The moving radio bursts, as well as other stationary bursts observed during the eruption, occur simultaneously with a type IV continuum in dynamic spectra, which is not usually associated with emission at the CME flanks. Our results show that moving radio bursts that could traditionally be classified as moving type IVs can represent shock signatures associated with CME flanks or plasma emission inside the CME behind its flanks, which are closely related to the lateral expansion of the CME in the low corona. In addition, the acceleration of electrons generating this radio emission appears to be favoured at the CME flanks, where the CME encounters coronal streamers and open field regions.

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Section: Observations and Data Analysismentioning

confidence: 99%

Three-dimensional reconstruction of multiple particle acceleration regions during a coronal mass ejection

Morosan

Palmerio

Pomoell

et al. 2020

A&A

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“…As shown in Figure 1, Earth and Venus were almost radially aligned during the passage of the CMEs; their longitudinal separation was 5.4 • and their latitudinal separation was 0.2 • . The solar and heliospheric characteristics of these CMEs, as well as some of their in-situ signatures (particularly those at Earth), have been investigated in several previous studies (e.g., Kubicka et al, 2016;James et al, 2017James et al, , 2018Palmerio et al, 2017;Srivastava et al, 2018;Pomoell et al, 2019;Scolini et al, 2019;Wang et al, 2019). Here, we focus on comparing interplanetary observations at Venus and Earth.…”

Section: Introductionmentioning

confidence: 99%

Multipoint Observations of the June 2012 Interacting Interplanetary Flux Ropes

Kilpua

Good

Palmerio

et al. 2019

Front. Astron. Space Sci.

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We report a detailed analysis of interplanetary flux ropes observed at Venus and subsequently at Earth's Lagrange L1 point between June 15 and 17, 2012. The observation points were separated by about 0.28 AU in radial distance and 5 • in heliographic longitude at this time. The flux ropes were associated with three coronal mass ejections (CMEs) that erupted from the Sun on June 12-14, 2012 (SOL2012-06-12, SOL2012-06-13, and SOL2012-06-14). We examine the CME-CME interactions using in-situ observations from the almost radially aligned spacecraft at Venus and Earth, as well as using heliospheric modeling and imagery. The June 14 CME reached the June 13 CME near the orbit of Venus and significant interaction occurred before they both reached Earth. The shock driven by the June 14 CME propagated through the June 13 CME and the two CMEs coalesced, creating the signatures of one large, coherent flux rope at L1. We discuss the origin of the strong interplanetary magnetic fields related to this sequence of events, the complexity of interpreting solar wind observations in the case of multiple interacting CMEs, and the coherence of the flux ropes at different observation points.

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“… 33 , 34 , 35 Twin dimmings are often believed to map the footpoints of the erupting flux rope. 31 , 32 , 36 , 37 , 38 In this paper, to identify the footpoint regions of the CME flux rope with a higher accuracy, we propose a new method that combines the previous two methods (see Material and Method for details). We show the results about the evolution of the toroidal flux during the eruption and give a discussion in the following.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the Toroidal Flux of CME Flux Ropes during Eruption

2020

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Summary Coronal mass ejections (CMEs) are large-scale explosions of the coronal magnetic field. It is believed that magnetic reconnection significantly builds up the core structure of CMEs, a magnetic flux rope, during the eruption. However, the quantitative evolution of the flux rope, particularly its toroidal flux, is still unclear. In this paper, we study the evolution of the toroidal flux of the CME flux rope for four events. The toroidal flux is estimated as the magnetic flux in the footpoint region of the flux rope, which is identified by a method that simultaneously takes the coronal dimming and the hook of the flare ribbon into account. We find that the toroidal flux of the CME flux rope for all four events shows a two-phase evolution: a rapid increasing phase followed by a decreasing phase. We further compare the evolution of the toroidal flux with that of the Geostationary Operational Environmental Satellites soft X-ray flux and find that they are basically synchronous in time, except that the peak of the former is somewhat delayed. The results suggest that the toroidal flux of the CME flux rope may be first quickly built up by the reconnection mainly taking place in the sheared overlying field and then reduced by the reconnection among the twisted field lines within the flux rope, as enlightened by a recent 3D magnetohydrodynamic simulation of CMEs.

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Evolution of a Magnetic Flux Rope toward Eruption

Cited by 32 publications

References 94 publications

Three-dimensional reconstruction of multiple particle acceleration regions during a coronal mass ejection

Three-dimensional reconstruction of multiple particle acceleration regions during a coronal mass ejection

Multipoint Observations of the June 2012 Interacting Interplanetary Flux Ropes

Evolution of the Toroidal Flux of CME Flux Ropes during Eruption

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