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

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 it has an additional stricking 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 in a medium where the magnetic field of the progenitor star is added to a constant galactic magnetic field. Also we have carried out a polarization study, obtaining synthetic maps of the linearly polarized intensity and the Stokes parameters, from our MHD results. This study reveals that both radio morphology and the reported RM for this remnant can be explained if the quasiparallel acceleration mechanism is taking place in the shock front of SNR G296.5+10.