  In the present work we have modeled the supernova remnant (SNR) G296.5+10, by
means of 3D magnetohydrodynamics (MHD) simulations. This remnant belongs to the
bilateral SNR group and has an additional striking feature: the rotation
measure (RM) in its eastern and western parts are very different. In order to
explain both the morphology observed in radio-continuum and the RM, we consider
that the remnant expands into a medium shaped by the superposition of the
magnetic field of the progenitor star with a constant Galactic magnetic field.
We have also carried out a polarization study from our MHD results, obtaining
synthetic maps of the linearly polarized intensity and the Stokes parameters.
This study reveals that both the radio morphology and the reported RM for
G$296.5+10$ can be explained if the quasi-parallel acceleration mechanism is
taking place in the shock front of this remnant.
