Temperature Evolution of a Magnetic Flux Rope in a Failed Solar Eruption

Song, Hongqiang; Zhang, J.; Cheng, X.; Chen, Yanlai; Liu, Rui; Wang, Y. M.; Li, B.

doi:10.1088/0004-637x/784/1/48

Cited by 55 publications

(55 citation statements)

References 44 publications

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“…For the remaining ones (17 of 26), like the 2013 January 5 event, the blob already had a considerable velocity or acceleration when it was first visible, without a detectable slow rise phase. We also compare the velocity evolution of the 2013 January 5 flare with the result of Song et al (2014) and find that they are consistent.…”

Section: Early Kinematic Evolutionmentioning

confidence: 54%

The Kinematic Evolution of Erupting Structures in Confined Solar Flares

Huang

Cheng

Ding

2020

ApJL

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In this Letter, we study the kinematic properties of ascending hot blobs associated with confined flares. Taking advantage of high-cadence extreme-ultraviolet images provided by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory, we find that for the 26 events selected here, the hot blobs are first impulsively accelerated outward, but then quickly slow down to motionlessness. Their velocity evolution is basically synchronous with the temporal variation of the Geostationary Operational Environmental Satellite soft X-ray flux of the associated flares, except that the velocity peak precedes the soft X-ray peak by minutes. Moreover, the duration of the acceleration phase of the erupting blobs is moderately correlated with that of the flare rise phase. For nine of the 26 cases, the erupting blobs even appear minutes prior to the onset of the associated flares. Our results show that a fraction of confined flares also involve the eruption of a magnetic flux rope, which sometimes is formed and heated prior to the flare onset. We suggest that the initiation and development of these confined flares are similar to that of eruptive ones, and the main difference may lie in the background field constraint, which is stronger for the former than for the latter.

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Section: Early Kinematic Evolutionmentioning

confidence: 54%

The Kinematic Evolution of Erupting Structures in Confined Solar Flares

Huang

Cheng

Ding

2020

ApJL

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“…The simulated loops rise somewhat during the main reconnection phase, then contract back down, so may be observed as "failed eruptions", which appear sometimes to be associated with kink instability (e.g. Alexander et al 2006;Song et al 2014). Flares can be directly associated with apparent instability of observed twisted flux ropes (e.g Wang et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Thermal and non-thermal emission from reconnecting twisted coronal loops

Pinto

Gordovskyy

Browning

et al. 2016

A&A

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Context. Twisted magnetic fields should be ubiquitous in the solar corona, particularly in flare-producing active regions where the magnetic fields are strongly non-potential. The magnetic energy contained in such twisted fields can be released during solar flares and other explosive phenomena. It has been shown recently that reconnection in helical magnetic coronal loops results in plasma heating and particle acceleration distributed within a large volume, including the lower coronal and chromospheric sections of the loops. Hence, the magnetic reconnection and particle acceleration scenario involving magnetic helicity can be a viable alternative to the standard flare model, where particles are accelerated only in a small volume located in the upper corona. Aims. The key goal of this study is to investigate the links and observational signatures of plasma heating and particle acceleration in kink-unstable twisted coronal loops. Methods. We use a combination of MHD simulations and test-particle methods. These simulations describe the development of kink instability and magnetic reconnection in twisted coronal loops using resistive compressible MHD, and incorporate atmospheric stratification and large-scale loop curvature. The resulting distributions of hot plasma let us estimate thermal X-ray emission intensities. The electric and magnetic fields obtained are used to calculate electron trajectories using the guiding-centre approximation. These trajectories combined with the MHD plasma density distributions let us deduce synthetic hard X-ray bremsstrahlung intensities. Results. Our simulations emphasise that the geometry of the emission patterns produced by hot plasma in flaring twisted coronal loops can differ from the actual geometry of the underlying magnetic fields. In particular, the twist angles revealed by the emission threads (soft X-ray thermal emission; SXR) are consistently lower than the field-line twist present at the onset of the kink-instability. Hard X-ray (HXR) emission due to the interaction of energetic electrons with the stratified background are concentrated at the loop foot-points in these simulations, even though the electrons are accelerated everywhere within the coronal volume of the loop. The maximum of HXR emission consistently precedes that of SXR emission, with the HXR light-curve being approximately proportional to the temporal derivative of the SXR light-curve.

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“…Therefore, sigmoid and HC might represent the same structure, their different shapes are likely from different perspectives and evolution phase. Both structures are featured by high temperature, a possible result of flare magnetic reconnection (e.g., Song et al 2014aSong et al , 2014b. Coronal cavity, on the other hand, observed as dark circular or oval structure above solar limb in coronal images with temperatures close to the background corona (Fuller et al 2008;Gibson et al 2010;Kucera et al 2012), is also interpreted as MFR.…”

Section: Introductionmentioning

confidence: 98%

The First Taste of a Hot Channel in Interplanetary Space

Song

Zhang

Chen

et al. 2015

ApJ

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Hot channel (HC) is a high temperature (∼10 MK) structure in the inner corona revealed first by Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory. Eruption of HC is often associated with flare and coronal mass ejection. Previous studies suggest that HC is a good proxy of magnetic flux rope (MFR) in the inner corona, in addition to another well-known MFR candidate, the prominence-cavity structure that is with a normal coronal temperature (∼1-2 MK). In this paper, we report a high temperature structure (HTS, ∼1.5 MK) contained in an interplanetary coronal mass ejection induced by an HC eruption. According to the observations of bidirectional electrons, high temperature and density, strong magnetic field, and its association with the shock, sheath, and plasma pile-up region, we suggest that the HTS is the interplanetary counterpart of the HC. The scale of the measured HTS is around 14 R ⊙ , and it maintained a much higher temperature than the background solar wind even at 1 AU. It is significantly different from the typical magnetic clouds (MCs), which usually have a much lower temperature. Our study suggests that the existence of a corotating interaction region ahead of the HC formed a magnetic container to inhibit the HC expansion and cooling down to a low temperature.

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Temperature Evolution of a Magnetic Flux Rope in a Failed Solar Eruption

Cited by 55 publications

References 44 publications

The Kinematic Evolution of Erupting Structures in Confined Solar Flares

The Kinematic Evolution of Erupting Structures in Confined Solar Flares

Thermal and non-thermal emission from reconnecting twisted coronal loops

The First Taste of a Hot Channel in Interplanetary Space

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