Geotail observations of the Kelvin‐Helmholtz instability at the equatorial magnetotail boundary for parallel northward fields

By D. Fairfield, A. Otto, T. Mukai, S. Kokubun, R. Lepping, J. Steinberg, A. Lazarus, T. Yamamoto. 2000

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Dawn‐dusk asymmetries, ion spectra, and sources in the northward interplanetary magnetic field plasma sheet (2005, background): “Signatures of these vortices have been found on the dusk flanks of the magnetosphere [e.g., Fairfield et al., 2000; Fujimoto et al., 2003].”
Single-spacecraft detection of rolled-up Kelvin-Helmholtz vortices at the flank magnetopause (2006, background): “According to the observed 2–3 min period and to the tailward flow speed of 150 km/s, the wavelength is estimated to be 3 to 4 RE, consistent with that reported in literature [e.g., Kivelson and Chen, 1995; Fairfield et al., 2000].”
Cluster observations of reconnection due to the Kelvin-Helmholtz instability at the dawnside magnetospheric flank (2006, background): “MHD simulations byOtto and Fairfield(2000) – motivated by Geotail observations of the KHI (Fairfield et al., 2000) – indicated that reconnection can occur inside the narrow current layers generated by the KHI at the flank magnetopause.”
Altered solar wind-magnetosphere interaction at low Mach numbers: Coronal mass ejections (2008, background): “Such observations were first interpreted in terms of enhanced magnetic tension of draped magnetic flux tubes that accelerate magnetosheath plasma along the magnetopause in the fashion of a magnetic “slingshot” [Chen et al., 1993].”