Energetic Electrons Associated with Magnetic Reconnection in the Magnetic Cloud Boundary Layer

Wang, Yi; Wei, Fengsi; Feng, Xueshang; Zhang, S. H.; Zuo, Pingbing; Sun, Tianran

doi:10.1103/physrevlett.105.195007

Cited by 39 publications

(22 citation statements)

References 31 publications

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“…With availability of higher time resolution datasets, larger numbers of candidate reconnection events have been identified [92]. There has been some controversy as to whether suprathermal particles are associated with some of these events [93,94]. At the same time, if we accept that a turbulence cascade is active in the interplanetary medium, then it seems inescapable that magnetic reconnection in some form must be ongoing.…”

Section: Evidence For Coherent Structures In the Solar Windmentioning

confidence: 99%

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Matthaeus

Wan

Servidio

et al. 2015

Phil. Trans. R. Soc. A.

183

139

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Section: Evidence For Coherent Structures In the Solar Windmentioning

confidence: 99%

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Matthaeus

Wan

Servidio

et al. 2015

Phil. Trans. R. Soc. A.

183

139

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“…However, few observations have confirmed the presence of energetic electrons in the reconnection exhaust of the magnetic cloud boundary layer [17]. In this paper, we report the first observation of energetic electrons within the exhaust in the sheath region of the ICME.…”

Section: Discussionmentioning

confidence: 67%

“…In fact, a region of energetic electron enhancement was also observed at only one pair of separatrices in the magnetic cloud boundary layer [17]. In addition, a kinetic simulation was conducted and a combined model (i.e.…”

Section: Discussionmentioning

confidence: 99%

“…In addition, a kinetic simulation was conducted and a combined model (i.e. electric field acceleration and Fermi-type mechanism) put forward to explain the origin of energetic electrons during magnetic reconnection there [17]. We also consider that a single acceleration mechanism is not enough to produce such high energy and so many energetic electrons during magnetic reconnection.…”

Section: Discussionmentioning

confidence: 99%

“…However, Gosling et al [16] found the absence of energetic particles associated with reconnection exhausts in the solar wind. Recently, Wang et al [17] presented the first evidence of energetic electrons associated with magnetic reconnection in the magnetic cloud boundary layer.…”

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confidence: 99%

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

et al. 2012

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Magnetic reconnection is an important universal plasma dissipation process that converts magnetic energy into plasma thermal and kinetic energy, and simultaneously changes the magnetic field topology. In this paper, we report the first observation of energetic electrons associated with asymmetric reconnection in the sheath of an interplanetary coronal mass ejection. The magnetic field shear angle was about 151°, implying guide-field reconnection. The width of the exhaust was about 8×10 4 km. The reconnection rate was estimated as 0.044-0.08, which is consistent with fast reconnection theory and previous observations. We observed flux enhancements of energetic electrons with energy up to 400 keV in this reconnection exhaust. The region where energetic electron fluxes were enhanced is located at one pair of separatrices in the higher density hemisphere. We discuss these observation results, and compare with previous observations and recent kinetic simulations.

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Geo‐effectiveness and radial dependence of magnetic cloud erosion by magnetic reconnection

et al. 2014

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[1] Magnetic flux erosion by magnetic reconnection occurs at the front of at least some magnetic clouds (MCs). We first investigate how erosion influences the geo-effectiveness of MCs in a general sense and using a south-north magnetic polarity MC observed on 18-20 October 1995. Although the magnetic shear at its front may not be known during propagation, measurements at 1 AU show signatures of local reconnection. Using a standard MC model, an empirical model of the geomagnetic response (Dst), and an observational estimate of the magnetic flux erosion, we find that the strength of the observed ensuing storm was~30% lower than if no erosion had occurred. We then discuss the interplay between adiabatic compression and magnetic erosion at the front of MCs. We conclude that the most geo-effective configuration for a south-north polarity MC is to be preceded by a solar wind with southward IMF. This stems not only from the formation of a geo-effective sheath ahead of it but also from the adiabatic compression and reduced (or lack thereof) magnetic erosion which constructively conspire for the structure to be more geo-effective. Finally, assuming simple semiempirical and theoretical Alfvén speed profiles expected from expansion to 1 AU, we provide first-order estimates of the erosion process radial evolution. We find that the expected reconnection rates during propagation allow for significant erosion, on the order of those reported. Calculations also suggest that most of the erosion should occur in the inner heliosphere, and up to~50% may yet occur beyond Mercury's orbit.

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Energetic Electrons Associated with Magnetic Reconnection in the Magnetic Cloud Boundary Layer

Cited by 39 publications

References 31 publications

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

Intermittency, nonlinear dynamics and dissipation in the solar wind and astrophysical plasmas

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

Geo‐effectiveness and radial dependence of magnetic cloud erosion by magnetic reconnection

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