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

Origin of the bilateral structure of the supernova remnant G296.5+10