By G. Venkataraman
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6 Schematic models of collapsing magnetic field lines occurring in MHD models of magnetic reconnection with (a) (dashed line) and without (b) a termination shock. From Somov and Kosugi (1997). 3) providing the secondary acceleration of electrons ejected from a current sheet. 1 Acceleration in Collapsing Magnetic Traps Somov and Kosugi (1997), Karlický and Kosugi (2004), and Bogachev and Somov (2005, 2007) have carried out simulations of the acceleration of electrons in collapsing magnetic traps for particles with an initial Maxwellian distribution that are injected at random points of a fragmented current sheet geometry obtained using a 3-D MHD simulation.
Sui and Holman, 2003), there is little direct evidence for the occurrence of these kinds of shocks near the top of flaring loops, where the acceleration seems to take place during the impulsive phase. Furthermore, such shocks typically do not appear in 3-D MHD simulations of the reconnection process. In summary, many of the features that make acceleration of cosmic rays by shocks attractive are not directly applicable to the solar flare environment and as a result have received only limited attention in the literature.
This again must be a property of either the magnetic field topology or a reconnecting current sheet. 11. , 2011). This can be related more to particle transport than to particle acceleration. 12. , 2011). This is assumed to be a property of particle transport combined with acceleration. 19 20 1 Observational Phenomena of Solar Flares 13. , 2011). This is assumed to be the property of particle transport combined with acceleration. 14. , 2011). This must be related to particle acceleration as well as to particle and emission transport.