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Particle acceleration in fast magnetic reconnection

Published online by Cambridge University Press:  08 June 2011

A. Lazarian ,
G. Kowal ,
E. de Gouveia Dal Pino  and
E. Vishniac
A. Lazarian
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI, 53706, USA, email: lazarian@astro.wisc.edu
G. Kowal
Affiliation:
Department of Astronomy of IAG, University of São Paulo, Rua do Matão, 1226, São Paulo, SP, 05508, Brazil Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Kraków, Poland
E. de Gouveia Dal Pino
Affiliation:
Department of Astronomy of IAG, University of São Paulo, Rua do Matão, 1226, São Paulo, SP, 05508, Brazil
E. Vishniac
Affiliation:
Department of Physics and Astronomy, McMaster University, 1280 Main St. W, Hamilton, ON, L8S 4M1, Canada
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Abstract

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Our numerical simulations show that the reconnection of magnetic field becomes fast in the presence of weak turbulence in the way consistent with the Lazarian & Vishniac (1999) model of fast reconnection. This process in not only important for understanding of the origin and evolution of the large-scale magnetic field, but is seen as a possibly efficient particle accelerator producing cosmic rays through the first order Fermi process. In this work we study the properties of particle acceleration in the reconnection zones in our numerical simulations and show that the particles can be efficiently accelerated via the first order Fermi acceleration.

Keywords

magnetic reconnectioncosmic raysacceleration
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 62 - 71
Copyright
Copyright © International Astronomical Union 2011

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