HR: 11:02h
AN: SH22A-03    [Abstracts]
TI: Proton acceleration by 3D magnetic reconnection in solar flares
AU: * Browning, P K
EM: p.browning@manchester.ac.uk
AF: School of Physics and Astronomy University of Manchester, Sackville Building , Manchester, M601QD, United Kingdom
AU: Dalla, S
EM: silvia.dalla@manchester.ac.uk
AF: School of Physics and Astronomy University of Manchester, Sackville Building , Manchester, M601QD, United Kingdom
AB: High energy charged particles are an important feature of solar activity such as flares, and indeed non thermal particles play a significant role in flare energy balance. Magnetic reconnection is the primary energy release mechanism in flares, and the strong DC electric fields associated with this reconnection may well be the origin of the high energy charged particles. Whilst particle acceleration has been widely studied for 2D configurations, little is known about 3D configurations. We investigate particle acceleration using a test particle approach, in the simplest 3D reconnection configuration, a 3D magnetic null point. Two modes of reconnection are possible: with a strong current filament along the "spine" field line connecting to the null, or with a sheet current at the "fan" plane of field lines emerging from the null. Using simple model fields, incorporating intiially only thee ideal reconnection region outside the current sheet (or filament), particle trajectories are investigated and the energy spectra and spatial distribution of accelerated particles are determined. We consider and compare fan and spine reconnection, and determine how the properties of the accelerated particles depend on the parameters of the reonnecting field. We also present preliminary results using more realistic, self consistent model fields.
DE: 7509 Corona
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7526 Magnetic reconnection (2723, 7835)
DE: 7807 Charged particle motion and acceleration
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly