Simultaneous Observation of a Flux Rope Eruption and Magnetic Reconnection during an X-class Solar Flare

Yan, Xiaoli; Yang, Liheng; Xue, Zhike; Mei, Zengxia; Kong, D. F.; Wang, J. C.; Li, Qiaoling

doi:10.3847/2041-8213/aaa6c2

Cited by 119 publications

(107 citation statements)

References 63 publications

Supporting

Mentioning

103

Contrasting

Unclassified

Order By: Relevance

“…Similar structures have often been identified as the flare current sheet by observers, and have been used to estimate the properties of the current sheet such as its width (e.g. Warren et al 2018;Yan et al 2018;Savage et al 2010).…”

Section: Euv and X-ray Emissionmentioning

confidence: 99%

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Reeves

Török

Mikić

et al. 2019

ApJ

View full text Add to dashboard Cite

We simulate a coronal mass ejection (CME) using a three-dimensional magnetohydrodynamic (MHD) code that includes coronal heating, thermal conduction, and radiative cooling in the energy equation. The magnetic flux distribution at 1 R s is produced by a localized subsurface dipole superimposed on a global dipole field, mimicking the presence of an active region within the global corona. Transverse electric fields are applied near the polarity inversion line to introduce a transverse magnetic field, followed by the imposition of a converging flow to form and destabilize a flux rope, producing an eruption. We examine the quantities responsible for plasma heating and cooling during the eruption, including thermal conduction, radiation, adiabatic effects, coronal heating, and ohmic heating. We find that ohmic heating is an important contributor to hot temperatures in the current sheet region early in the eruption, but in the late phase adiabatic compression plays an important role in heating the plasma there. Thermal conduction also plays an important role in the transport of thermal energy away from the current sheet region throughout the reconnection process, producing a "thermal halo" and widening the region of high temperatures. We simulate emission from solar telescopes for this eruption and find that there is evidence for emission from heated plasma above the flare loops late in the eruption, when the adiabatic heating is the dominant heating term. These results provide an explanation for hot supra-arcade plasma sheets that are often observed in X-rays and extreme ultraviolet wavelengths during the decay phase of large flares.

show abstract

Section: Euv and X-ray Emissionmentioning

confidence: 99%

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Reeves

Török

Mikić

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…It usually occurs at null points, current sheets, or the quasiseparatrix layers. Magnetic reconnection is generally considered to be associated with solar activities, for example, flares, coronal mass ejections, filament eruptions, and jets (Shibata et al 1992;Sturrock 1966;Lin & Forbes 2000;Moore et al 2001;Yan et al 2018;Cheng et al 2018). Magnetic reconnection can cause coronal condensation and helical structure, which may result in the formation of filament or prominence (Kaneko & Yokoyama 2017;Li et al 2018Li et al , 2019Xue et al 2017).…”

Section: Introductionmentioning

confidence: 99%

A solar filament disconnected by magnetic reconnection

Xue

Yan

Yang

et al. 2020

A&A

View full text Add to dashboard Cite

Aims. We aim to study a high-resolution observation of an asymmetric inflow magnetic reconnection between a filament and its surrounding magnetic loops in active region NOAA 12436 on 2015 October 23. Methods. We analyzed the multiband observations of the magnetic reconnection obtained by the New Vacuum Solar Telescope (NVST) and the Solar Dynamic Observatory. We calculated the NVST Hα Dopplergrams to determine the Doppler properties of the magnetic reconnection region and the rotation of a jet. Results. The filament firstly becomes active and then approaches its southwestern surrounding magnetic loops (L1) with a velocity of 9.0 km s−1. During this period, the threads of the filament become loose in the reconnection region and then reconnect with L1 in turn. L1 is pressed backward by the filament with a velocity of 5.5 km s−1, and then the magnetic reconnection occurs between them. A set of newly formed loops are separated from the reconnection site with a mean velocity of 127.3 km s−1. In the middle stage, some threads of the filament return back first with a velocity of 20.1 km s−1, and others return with a velocity of 4.1 km s−1 after about 07:46 UT. Then, L1 also begins to return with a velocity of 3.5 km s−1 at about 07:47 UT. At the same time, magnetic reconnection continues to occur between them until 07:51 UT. During the reconnection, a linear typical current sheet forms with a length of 5.5 Mm and a width of 1.0 Mm, and a lot of hot plasma blobs are observed propagating from the typical current sheet. During the reconnection, the plasma in the reconnection region and the typical current sheet always shows redshifted feature. Furthermore, the material and twist of the filament are injected into the newly longer-formed magnetic loops by the magnetic reconnection, which leads to the formation of a jet, and its rotation. Conclusions. The observational evidence for the asymmetric inflow magnetic reconnection is investigated. We conclude that the magnetic reconnection does occur in this event and results in the disconnection of the filament. The looseness of the filament may be due to the pressure imbalance between the inside and outside of the filament. The redshifted feature in the reconnection site can be explained by the expansion of the right flank of the filament to the lower atmosphere because of the complex magnetic configuration in this active region.

show abstract

“…The global EUV wave was accompanied by an X8.2 flare and a violent CME driving a shock on the west limb of the Sun on 2017 September 10, which was observed by spacecraft on the opposite sides of the Sun. The related coronal and interplanetary properties have been studied in several works (e.g., Seaton & Darnel 2018;Li et al 2018;Yan et al 2018;Goryaev et al 2018;Luhmann et al 2018;Liu et al 2018;Cheng et al 2018;Liu et al 2019). In this paper we analyze the observations of Solar Terrestrial Relations Observatory A (STEREO-A), Solar Dynamics Observatory (SDO), Geostationary Operational Environmental Satellite 16 (GOES-16 ), and Solar and Heliospheric Observatory (SOHO) from nearly opposite sides of the Sun.…”

Section: Introductionmentioning

confidence: 99%

Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

Liu

Zhu

et al. 2019

ApJ

View full text Add to dashboard Cite

We investigate a global extreme-ultraviolet (EUV) wave associated with a coronal mass ejection (CME)-driven shock on 2017 September 10. The EUV wave is transmitted by north-and south-polar coronal holes (CHs), which is observed by the Solar Dynamics Observatory (SDO) and Solar Terrestrial Relations Observatory A (STEREO-A) from opposite sides of the Sun. We obtain key findings on how the EUV wave interacts with multiple coronal structures, and on its connection with the CME-driven shock:(1) the transmitted EUV wave is still connected with the shock that is incurvated to the Sun, after the shock has reached the opposite side of the eruption; (2) the south CH transmitted EUV wave is accelerated inside an on-disk, low-density region with closed magnetic fields, which implies that an EUV wave can be accelerated in both open and closed magnetic field regions; (3) part of the primary EUV wavefront turns around a bright point (BP) with a bipolar magnetic structure when it approaches a dim, low-density filament channel near the BP; (4) the primary EUV wave is diffused and apparently halted near the boundaries of remote active regions (ARs) that are far from the eruption, and no obvious AR related secondary waves are detected; (5) the EUV wave extends to an unprecedented scale of ∼360 • in latitudes, which is attributed to the polar CH transmission. These results provide insights into the effects of coronal density and magnetic field distributions on the evolution of an EUV wave, and into the connection between the EUV wave and the associated CME-driven shock.

show abstract

Simultaneous Observation of a Flux Rope Eruption and Magnetic Reconnection during an X-class Solar Flare

Cited by 119 publications

References 63 publications

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

Exploring Plasma Heating in the Current Sheet Region in a Three-dimensional Coronal Mass Ejection Simulation

A solar filament disconnected by magnetic reconnection

Effects of Coronal Density and Magnetic Field Distributions on a Global Solar EUV Wave

Contact Info

Product

Resources

About