Energetic electron acceleration in the downstream reconnection outflow region

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Ion heating resulting from pickup in magnetic reconnection exhausts (2009, background): “energetic electrons seen during reconnection in the magnetotail [Øieroset et al., 2002; Imada et al., 2007; Chen et al., 2008]? An obvious difference between the corona and the solar wind and magnetotail is the ambient plasma b, which is very small in the corona.”
Particle Acceleration in the Magnetotail and Aurora (2012, methodology): “As reported by Cluster observations (Imada et al. 2007), in addition to the Speiser/meandering particle acceleration in the X-type region, energetic electrons can be further accelerated in the magnetic field pileup region produced by compression of the reconnection outflow.”
Average properties of the magnetic reconnection ion diffusion region in the Earth's magnetotail: The 2001–2005 Cluster observations and comparison with simulations (2009, background): “The properties of the Hall magnetic field [Runov et al., 2003], Hall electric field [Wygant et al., 2005], energetic particles [Imada et al., 2007; Chen et al., 2008], and electrostatic structures [Cattell et al., 2005] have all been examined.”