Abstract
Observational data require a rich variety of mechanisms to accelerate fast particles in astrophysical environments operating under different conditions. The mechanisms discussed in the literature include varying magnetic fields in compact sources, stochastic processes in turbulent environments, and acceleration behind shocks. An alternative, much less explored mechanism involves particle acceleration within magnetic reconnection sites. In this chapter we discuss this mechanism and show that particles can be efficiently accelerated by magnetic reconnection through a first order Fermi process within large scale current sheets (specially when in the presence of local turbulence which speeds up the reconnection and make the acceleration region thicker) and also through a second order Fermi process in pure MHD turbulent environments.
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Acknowledgements
E.M.G.D.P. acknowledges partial support from the Brazilian agencies FAPESP (grant no. 2006/50654-3 and CNPq (grant no. 300083/94-7) and G.K. also acknowledges support from FAPESP (grant 2009/50053-8). The authors are also in debt to Alex Lazarian for fruitful and joyful collaboration in this work. Part of the simulations presented here have been carried out in LAI (Astrophysical Laboratory of Informatics at IAG-USP).
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de Gouveia Dal Pino, E.M., Kowal, G. (2015). Particle Acceleration by Magnetic Reconnection. In: Lazarian, A., de Gouveia Dal Pino, E., Melioli, C. (eds) Magnetic Fields in Diffuse Media. Astrophysics and Space Science Library, vol 407. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-44625-6_13
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