Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection

Huang, Suming; Deng, Xiaohua; Zhou, Meng; Yuan, Zhigang; Li, Huimin; Wang, Dedong

doi:10.1007/s11434-012-4974-9

Cited by 9 publications

(5 citation statements)

References 28 publications

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“…Energetic electrons with energies of hundreds of keV have been observed in the reconnection diffusion region [ Øieroset et al , 2002; He et al , 2008; Retinò et al , 2008], outflow region [ Imada et al , 2007; Huang et al , 2012], and within magnetic islands [ Chen et al , 2008; Retinò et al , 2008; Wang et al , 2010]. Recently, Imada et al [2011] have studied favorable conditions for energetic electron acceleration using 10 reconnection events observed by Geotail, and found that the electrons are efficiently accelerated in a thin CS during magnetic reconnection.…”

Section: Discussionmentioning

confidence: 99%

“…Energetic electrons are important consequences of magnetic reconnection [e.g., Hoshino et al , 2001; Drake et al , 2006a; Pritchett , 2006], and have been observed associated with reconnection [e.g., Øieroset etal. , 2002; Imada et al , 2007; Retinò et al , 2008; Huang et al , 2012]. Magnetic islands are closely related to electron acceleration during reconnection.…”

Section: Introductionmentioning

confidence: 99%

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Electron acceleration in the reconnection diffusion region: Cluster observations

Huang

Vaivads

Khotyaintsev

et al. 2012

Geophysical Research Letters

107

128

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[1] We present one case study of magnetic islands and energetic electrons in the reconnection diffusion region observed by the Cluster spacecraft. The cores of the islands are characterized by strong core magnetic fields and density depletion. Intense currents, with the dominant component parallel to the ambient magnetic field, are detected inside the magnetic islands. A thin current sheet is observed in the close vicinity of one magnetic island. Energetic electron fluxes increase at the location of the thin current sheet, and further increase inside the magnetic island, with the highest fluxes located at the core region of the island. We suggest that these energetic electrons are firstly accelerated in the thin current sheet, and then trapped and further accelerated in the magnetic island by betatron and Fermi acceleration.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Electron acceleration in the reconnection diffusion region: Cluster observations

Huang

Vaivads

Khotyaintsev

et al. 2012

Geophysical Research Letters

107

128

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“…However, the net energy increment of this trapped cold ion is only 𝐴𝐴 ∼ 0.08 𝑚𝑚𝑖𝑖𝑣𝑣 2 𝐴𝐴 at 𝐴𝐴 𝐴𝐴= 47.5 . Previous studies suggest that electrons can be energized significantly in secondary islands (e.g., Huang et al, 2012;Zhong et al, 2020). Here we do not see obvious electron energization within this secondary island, similar to cold ions.…”

Section: Energization By Reconnectionmentioning

confidence: 99%

Energization of Cold Ions in Magnetic Reconnection: Particle‐in‐Cell Simulation

Song

Zhou

et al. 2022

JGR Space Physics

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Cold ions in the ionosphere can reach the nightside magnetotail along the magnetic field lines, which may substantially affect the magnetotail reconnection and reconnection‐driven phenomena. Although reconnection has been intensively studied in the past decades, the dynamics of cold ions in reconnection are poorly known. We performed a 2.5‐D full kinetic simulation to study the energization of cold ions in a symmetric anti‐parallel reconnection. We find that the cold ions can be considerably energized during reconnection. The average energy gain per cold ion is smaller than that per hot ion but larger than that per electron. The cold ions with the highest energy are firstly accelerated around the X‐line, and further accelerated around the reconnection front in the outflow region. They perform the meandering motion at the X‐line, while simultaneously accelerated by the reconnection out‐of‐plane electric field. The velocity distribution of cold ions around the X‐line is characterized by the counter‐streaming inflow component and the accelerated component in the +y quadrant. The cold ions are picked up at the reconnection front and trapped by the secondary island, resulting in a bump in the energy spectrum. The energy of the bump is close to the energy of the propagating speed of the reconnection front and the secondary island. Furthermore, a crescent‐shaped velocity distribution is observed at the reconnection front, caused by the finite Larmor radius effect of the high‐energy cold ions in the flux pileup region. Our result presents an important building block toward a fully understanding of the magnetosphere‐ionosphere coupling.

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“…2003; Gosling et al 2007;Wang et al 2010;Chian & Muñoz 2011) and numerical experiments (e.g., Schmidt & Cargill 2003;Wang et al 2010) that magnetic reconnection can occur at the interface between the leading edge of interplanetary coronal mass ejections (ICMEs) and background solar wind magnetic field (see also Démoulin 2008). Such episodes of magnetic reconnection could supply beams of suprathermal and/or nonthermal energetic electrons to the sheath region (Wang et al 2010;Huang et al 2012), thus possibly creating the necessary conditions for generation of the Langmuir turbulence and radio emission there. However, we realize (and emphasize) that this important issue requires further studies.…”

Section: Scenariomentioning

confidence: 99%

Spatially resolved observations of a split-band coronal type II radio burst

Zimovets

Vilmer

Chian

et al. 2012

A&A

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Context. The origin of coronal type II radio bursts and the nature of their band splitting are still not fully understood, though a number of scenarios have been proposed to explain them. This is largely due to the lack of detailed spatially resolved observations of type II burst sources and of their relations to magnetoplasma structure dynamics in parental active regions. Aims. To make progress in solving this problem on the basis of one extremely well observed solar eruptive event.Methods. The relative dynamics of multithermal eruptive plasmas, observed in detail by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, and of harmonic type II burst sources, observed by the Nançay Radioheliograph at ten frequencies from 445 to 151 MHz, was studied for the 3 November 2010 event arising from an active region behind the east solar limb. Special attention was given to the band splitting of the burst. Analysis was supplemented by investigation of coronal hard X-ray (HXR) sources observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager. Results. We found that the flare impulsive phase was accompanied by the formation of a double coronal HXR source, whose upper part coincided with the hot (T ≈ 10 MK) eruptive plasma blob. The leading edge (LE) of the eruptive plasmas (T ≈ 1−2 MK) moved upward from the flare region with a speed of v ≈ 900−1400 km s −1 . The type II burst source initially appeared just above the LE apex and moved with the same speed and in the same direction. After ≈20 s, it started to move about twice as fast, but still in the same direction. At any given moment, the low-frequency component (LFC) source of the splitted type II burst was situated above the highfrequency component (HFC) source, which in turn was situated above the LE. We also found that at a given frequency the HFC source was located slightly closer to the photosphere than the LFC source. Conclusions. Based on the set of established observational facts, we conclude that the shock wave, which could be responsible for the observed type II radio burst, was initially driven by the multi-temperature eruptive plasmas, but later transformed to a freely propagating blast shock wave. The preferable interpretation of the type II burst splitting is that its LFC was emitted from the upstream region of the shock, whereas the HFC was emitted from the downstream region. The shock wave in this case could be subcritical.

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Energetic electrons associated with magnetic reconnection in the sheath of interplanetary coronal mass ejection

Cited by 9 publications

References 28 publications

Electron acceleration in the reconnection diffusion region: Cluster observations

Electron acceleration in the reconnection diffusion region: Cluster observations

Energization of Cold Ions in Magnetic Reconnection: Particle‐in‐Cell Simulation

Spatially resolved observations of a split-band coronal type II radio burst

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