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3-D hybrid simulations (ion particle, charge neutralizing massless electron fluid) of magnetic reconnection in a thin current sheet (thickness comparable to the relevant ion inertia length) are conducted.
The polarization electric field in a thin current sheet can also contribute to electron pre-acceleration.
Their finding is that the energetic electrons are efficiently accelerated in a thin current sheet during fast reconnection events.
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Arridge et al. (2007) has interpreted Cassini magnetometer observations as a thin current sheet in the form of a magnetodisc.
The current density peak in the separatrix region implies that a thin current sheet is formed apart from the neutral line, which can evolve to the bifurcated current sheet.
We have demonstrated that the out-of-plane current density has a peak near the electron separatrix, which implies that a thin current sheet formed in the separatrix region.
Similar to the 2-D PIC simulations, the onset and dynamic phase was preceded by a driven phase (t<t 0, with t 0=61 in the chosen dimensionless units of ∼10 s)., during which a finite amount of magnetic flux was added at the high-latitude boundaries, causing compression and the formation of <span class="lh">a thin current sheet, embedded in the wider plasma sheet.
For a simple dipolar solar magnetic field, with opposite hemispherical polarities on either side of the solar magnetic equator, a thin current sheet is formed in the solar wind.
At steady state, the fluid motion was in accordance with Darcy's law for horizontal flow in a long thin current.
In contrast, in the separatrix region, the magnetic fields are not reversed in the thin current sheet, and the accelerated electrons make cyclotron motions rather the meandering motions.
(1) As shown previously in the literature, near-earth instabilities and reconnection usually take place in thin current sheet conditions (Büchner and Kuska 1999; Drake et al. 1994; Nakamura et al. 2006; Schindler and Birn 1993, 1999).
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