Observation of energetic electrons within magnetic islands

Chen, Li‐Jen; Bhattacharjee, A.; Puhl-Quinn, P.; Yang, Hang; Bessho, Naoki; Imada, Shinsuke; Mühlbachler, S.; Daly, P. W.; Lefebvre, Bertrand; Khotyaintsev, Yuri V.; Vaivads, A.; Fazakerley, A. N.; Georgescu, E.

doi:10.1038/nphys777

Cited by 252 publications

(302 citation statements)

References 25 publications

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“…Electron energization at magnetid islands has been reported with the Cluster observations during reconnections in the Earth's magnetosphere [122][123][124]. This provides support to the above scenarios.…”

Section: Studies On Magnetic Islands Of Reconnections Along the Cme Csupporting

confidence: 66%

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Chen

2013

Chin. Sci. Bull.

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In this article I present a review of recent studies on coronal dynamics, including research progresses on the physics of coronal streamers that are the largest structure in the corona, physics of coronal mass ejections (CMEs) that may cause a global disturbance to the corona, as well as physics of CME-streamer interactions. The following topics will be discussed in depth: (1) acceleration of the slow wind flowing around the streamer considering the effect of magnetic flux tube curvature; (2) physical mechanism accounting for persistent releases of streamer blobs and diagnostic results on the temporal variability of the slow wind speed with such events; (3) force balance analysis and energy release mechanism of CMEs with a flux rope magnetohydrodynamic model; (4) statistical studies on magnetic islands along the coronal-ray structure behind a CME and the first observation of magnetic island coalescence with associated electron acceleration; and (5) white light and radio manifestations of CME-streamer interactions. These studies shed new light on the physics of coronal streamers, the acceleration of the slow wind, the physics of solar eruptions, the physics of magnetic reconnection and associated electron acceleration, the large-scale coronal wave phenomenon, as well as the physics accounting for CME shock-induced type II radio bursts. solar wind, coronal streamer, coronal mass ejection, solar radio burst, magnetic reconnection Citation:Chen Y. A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions.

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Section: Studies On Magnetic Islands Of Reconnections Along the Cme Csupporting

confidence: 66%

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Chen

2013

Chin. Sci. Bull.

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“…More evidence of Hall physics was observed at the magnetopause where satellite data were used to show that the diffusion region is stable on the ion time scale (Mozer et al, 2002;Vaivads et al, 2004). Recently, coherent magnetic structures (or magnetic islands) with typical dimensions of the order of the ion inertial length and their link to the generation of energetic suprathermal electrons were observed by the Cluster quartet in the Magnetotail (Chen et al, 2008). In situ evidence of magnetic reconnection was even observed in thin current sheets forming inside the turbulent magnetosheath, downstream of a collisionless quasi-parallel shock period (Retinó et al, 2007).…”

Section: F Califano Et Al: Solar Wind Interaction With the Earth's mentioning

confidence: 99%

Solar wind interaction with the Earth's magnetosphere: the role of reconnection in the presence of a large scale sheared flow

Califano

Faganello

Пегораро

et al. 2009

Nonlin. Processes Geophys.

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Abstract. The Earth's magnetosphere and solar wind environment is a laboratory of excellence for the study of the physics of collisionless magnetic reconnection. At low latitude magnetopause, magnetic reconnection develops as a secondary instability due to the stretching of magnetic field lines advected by large scale Kelvin-Helmholtz vortices. In particular, reconnection takes place in the sheared magnetic layer that forms between adjacent vortices during vortex pairing. The process generates magnetic islands with typical size of the order of the ion inertial length, much smaller than the MHD scale of the vortices and much larger than the electron inertial length. The process of reconnection and island formation sets up spontaneously, without any need for special boundary conditions or initial conditions, and independently of the initial in-plane magnetic field topology, whether homogeneous or sheared.

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“…[5,7,16,17] However, electrical fields within a small fraction of the total volume at X lines are difficult to account for the large number of accelerated electrons of the total volume. [18] Recently Chen et al [18] reported some surprising satellite observation evidences that energetic electron flux peaks at sites of compressed density within islands during electon-ion reconnection in the Earth's magnetosphere. Hesse and Zenitani [14] reported that for relativistic pair plasmas in 2D without a guide field, most of particle acceleration happens inside magnetic islands possibly like a betatron (but no details are provided) (also see Dmitruk, Matthaeus and Seenu [19]).…”

Section: Introductionmentioning

confidence: 99%

Particle energization in 3D magnetic reconnection of relativistic pair plasmas

Liu

Yin

et al. 2011

Physics of Plasmas

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We present large scale 3D particle-in-cell (PIC) simulations to examine particle energization in magnetic reconnection of relativistic electron-positron (pair) plasmas.The initial configuration is set up as a relativistic Harris equilibrium without a guide field. These simulations are large enough to accommodate a sufficient number of tearing and kink modes. Contrary to the non-relativistic limit, the linear tearing instability is faster than the linear kink instability, at least in our specific parameters.We find that the magnetic energy dissipation is first facilitated by the tearing instability and followed by the secondary kink instability. Particles are mostly energized inside the magnetic islands during the tearing stage due to the spatially varying electric fields produced by the outflows from reconnection. Secondary kink instability leads to additional particle acceleration. Accelerated particles are, however, observed to be thermalized quickly. The large amplitude of the vertical magnetic field resulting from the tearing modes by the secondary kink modes further help thermalizing the non-thermal particles generated from the secondary kink instability. Implications of these results for astrophysics are briefly discussed.

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Observation of energetic electrons within magnetic islands

Cited by 252 publications

References 25 publications

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

Solar wind interaction with the Earth's magnetosphere: the role of reconnection in the presence of a large scale sheared flow

Particle energization in 3D magnetic reconnection of relativistic pair plasmas

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