Abstract
ABSTRACT We examine the evolution and emission of the supernova remnant (SNR) CTB 109 using 3D magnetohydrodynamics simulations. The SNR evolves in a medium divided by a plane interface into two media with different densities and pressure equilibrium. Our results reveal that a remnant with the characteristics of CTB 109 is formed provided the supernova (SN) explosion takes place in the less dense medium and also if the interstellar magnetic field (ISMF) is almost uniform. Finally, we conclude that the quasi-parallel mechanism can explain the brightness synchrotron emission and the position angle of the projected ISMF reported in previous works.
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