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Synergy of stochastic and systematic energization of plasmas during turbulent reconnection by Th. Pisokas, L. Vlahos and H. Isliker

6 Feb 2018, 10:06 UTC
Synergy of stochastic and systematic energization of plasmas during turbulent reconnection  by Th. Pisokas, L. Vlahos and H. Isliker
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In the current literature the acceleration of particles during solar flares is attributed to either weak turbulence or to large scale Unstable Current Sheet (UCS). The way UCS drive weak turbulence in a separated volume on the loop top or inside the loops below the UCS was never been presented in detail. During the last thirty years the plasma physics community developed the concept of turbulent reconnection. This concept went unnoticed in the solar physics community, mainly because the possibility that strong turbulence being present in the solar corona, especially during large scale explosions (flares, CMEs), had never been discussed in detail.
Figure 1. (a) Current density (colour) and magnetic field lines, possible reconnection sites are indicated by crosses. (b) The proton temperature (colour). [Servidio, et al., . 2009]
Turbulent reconnection can be generated by different, well known, non-linear MHD processes and structures, which serve as their driver, e.g. the evolution of a spectrum of large amplitude MHD waves, the fragmentation of a current sheet(s), or shock(s), the emerging magnetic flux or the kink instability of unstable loops. Several authors explored the formation of turbulent reconnection in the solar atmosphere, driven by the turbulent convection zone e.g. Parker (1983, 1988), ...

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