The magnetic fields can change their topology through a process known as
magnetic reconnection. This process in not only important for understanding
the origin and evolution of the large-scale magnetic field, but is seen as a
possibly efficient particle accelerator producing cosmic rays mainly through
the first order Fermi process. In my seminar I will present our work on
understanding the properties of particle acceleration inserted in reconnection
zones and show that the velocity component parallel to the magnetic field of
test particles injected in magnetohydrodynamic (MHD) domains of reconnection
without including kinetic effects, such as pressure anisotropy, the Hall term,
or anomalous effects, increases exponentially.  Also, the acceleration of the
perpendicular component is always possible in such models.  Within contracting
magnetic islands or current sheets the particles accelerate predominantly
through the first order Fermi process, as previously described, while outside
the current sheets and islands the particles experience mostly drift
acceleration due to magnetic fields gradients.  The importance of inclusion of
a guide field or performing fully three dimensional studies for a complete
understanding of the process of particle acceleration in astrophysical
reconnection environments is demonstrated as well.