Quadrupolar pattern of the asymmetric guide‐field reconnection

Peng, Fang‐Zheng; Fu, H. S.; Cao, Jinbin; Graham, Daniel B.; Chen, Z. Z.; Cao, Dairong; Xu, Yuanyuan; Huang, Suming; Wang, T. Y.; Khotyaintsev, Yuri V.; André, Mats; Russell, C. T.; Giles, B. L.; Lindqvist, Per‐Arne; Torbert, R. B.; Ergun, R. E.; Burch, J. L.

doi:10.1002/2016ja023666

Cited by 44 publications

(34 citation statements)

References 50 publications

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“…The situation is the same for the n = 1 mode. This result is consistent with previous observations showing clear bipolar (Mozer et al, ) and quadrupolar (Peng et al, ) patterns of Hall magnetic field in the presence of a large guide field.…”

Section: Theoretical Analysissupporting

confidence: 94%

Structures of Hall Fields in Asymmetric Magnetic Reconnection

Dai

2018

JGR Space Physics

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Unlike a quadrupolar Hall magnetic field in symmetric magnetic reconnection, a bipolar or quadrupolar Hall magnetic field occurs in asymmetric reconnection as indicated by recent observations from the Magnetospheric Multiscale (MMS) mission. Here we present analytic calculations of the structures of Hall magnetic fields in asymmetric reconnection. The Hall magnetic fields are analyzed in terms of kinetic Alfvén wave eigenmodes of the reconnection layer. The bipolar and quadrupolar patterns of Hall magnetic fields correspond to a dominance of the n = 0 and n = 1 kinetic Alfvén wave eigenmode, respectively. The asymmetry of Hall fields is linked to the asymmetry of the Alfvé speed profile. The Hall magnetic fields are shifted toward and enhanced on the low Alfvén speed side of the reconnection layer. The asymmetry in the magnetic field strength of the reconnection layer has a major effect on the structures of Hall magnetic fields.

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Section: Theoretical Analysissupporting

confidence: 94%

Structures of Hall Fields in Asymmetric Magnetic Reconnection

Dai

2018

JGR Space Physics

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“…Since the plasma density in the magnetosheath is significantly larger than that in the magnetosphere (Figure b), and also, the magnetic field in the magnetosheath is weaker than that in the magnetosphere (Figure a), this reconnection event was asymmetric (see Figure i). During such asymmetric reconnection, the quadrupolar pattern of Hall reconnection is still seen (Figure d), consistent with that reported by Peng et al ().…”

Section: Observation Of Magnetopause Reconnectionsupporting

confidence: 91%

Evidence of Electron Acceleration at a Reconnecting Magnetopause

Peng

Liu

et al. 2019

Geophysical Research Letters

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It is still unknown nowadays whether magnetic reconnection—a process occurring both in the magnetotail and at the magnetopause—can intrinsically accelerate energetic electrons. Observations in the Earth's magnetotail usually indicate strong electron acceleration during magnetic reconnection, while observations at the Earth's magnetopause rarely show such features. With the recently launched Magnetospheric Multiscale (MMS) mission, here we report the first evidence of energetic‐electron acceleration at a reconnecting magnetopause. We find that the acceleration of electrons, with energy up to 70 times their thermal energy, occurs in the magnetosheath side of the ion diffusion region and is associated with strong whistler waves. Such acceleration—not contaminated by the magnetospheric population—is attributed to nonadiabatic wave‐particle interactions, as supported by analyses of the resonance condition. It manifests that energetic‐electron acceleration can happen at the reconnecting magnetopause, like that in the tail.

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“…In this study, we focus on magnetotail reconnection that falls into collisionless plasma regime in which fast magnetic reconnection is controlled by the Hall effect (e.g., Birn et al, 2001;Eastwood et al, 2010;Fu et al, 2006;Lu et al, 2010;Peng et al, 2017). In collisional regime, chains of plasmoids had also been found formed, which is crucial to collisional fast reconnection based on magnetohydrodynamic theory and simulations (e.g., Bhattacharjee et al, 2009;Loureiro et al, 2007;Pucci & Velli, 2014;Samtaney et al, 2009;Tenerani et al, 2015) and then later examined using PIC simulations (e.g., Daughton et al, 2009aDaughton et al, , 2009b.…”

Section: Geophysical Research Lettersmentioning

confidence: 99%

Effects of Cross‐Sheet Density and Temperature Inhomogeneities on Magnetotail Reconnection

Artemyev

Angelopoulos

et al. 2019

Geophysical Research Letters

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Properties of magnetic reconnection in Earth's magnetotail are determined by prereconnection current sheet characteristics. Although spacecraft observations have revealed that the spatial profiles of two important parameters, density and temperature, across the prereconnection magnetotail current sheet are inhomogeneous, the effects of the inhomogeneities on reconnection processes have received insufficient attention. Using Time History of Events and Macroscale Interactions during Substorm (THEMIS) and Acceleration, Reconnection, Turbulence, and Electrodynamics of Moon's Interaction with the Sun (ARTEMIS) observations, we show that the inhomogeneities are ubiquitous throughout the magnetotail. Using particle‐in‐cell simulations, we demonstrate that strong density inhomogeneity increases magnetotail reconnection rate, and strong temperature inhomogeneity further increases reconnection outflow speed (although reconnection rate does not change significantly). Overall, these inhomogeneities expedite energy conversion efficiency and secondary plasmoid formation during reconnection. As the current sheet density and temperature characteristics vary considerably with geocentric distance and time under different geospace conditions, a large variety of reconnection and postreconnection dynamics results from this dependence.

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Quadrupolar pattern of the asymmetric guide‐field reconnection

Cited by 44 publications

References 50 publications

Structures of Hall Fields in Asymmetric Magnetic Reconnection

Structures of Hall Fields in Asymmetric Magnetic Reconnection

Evidence of Electron Acceleration at a Reconnecting Magnetopause

Effects of Cross‐Sheet Density and Temperature Inhomogeneities on Magnetotail Reconnection

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