Abstract

Secondary flux ropes are suggested to play important roles in energy dissipation and particle acceleration during magnetic reconnection. However, their generation mechanism is not fully understood. In this Letter, we present the first direct evidence that a secondary flux rope was generated due to the evolution of an electron vortex, which was driven by the electron Kelvin-Helmholtz instability in an ion diffusion region as observed by the Magnetospheric Multiscale mission. The subion scale (less than the ion inertial length) flux rope was embedded within the electron vortex, which contained a secondary electron diffusion region at the trailing edge of the flux rope. We propose that intense electron shear flow produced by reconnection generated the electron Kelvin-Helmholtz vortex, which induced a secondary reconnection in the exhaust of the primary X line and then led to the formation of the flux rope. This result strongly suggests that secondary electron Kelvin-Helmholtz instability is important for reconnection dynamics.

Highlights

  • The generation of secondary flux ropes (FRs) is not fully understood yet

  • In this Letter, we present the first direct evidence that a secondary flux rope was generated due to the evolution of an electron vortex, which was driven by the electron Kelvin-Helmholtz instability in an ion diffusion region as observed by the Magnetospheric Multiscale mission

  • Kinetic simulations show that secondary FR can be generated by electron vortex, which is a nonlinear consequence of electron KelvinHelmholtz (K-H) instability driven by electron shear flows produced during magnetic reconnection [10,11]

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Summary

FR FR

During this interval, MMS observed a flow reversal in ViL from −250 to 160 km/s. MMS observed a flow reversal in ViL from −250 to 160 km/s This indicates that a reconnection X line passed the MMS along the -L direction. Magnetic field BL component of MMS4 changed from negative to positive, and returned back to negative This indicates that MMS4 crossed the MP from the magnetosheath (BL < 0) to the magnetosphere (BL > 0), and moved back to the magnetosheath. One FR was detected in the magnetosheath side of the MP and the other one was detected in the MP current sheet Both FRs were manifested by the bipolar variations in BN [Fig. 1(e)] and enhancements in the out-of-plane component BM [Fig. 1(d)]. Similar to the FR, these large amplitude flows were not detected by the other three spacecraft

Jpara Jperp
Time axis
BL BM BN VL VM VN
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