  We performed three-dimensional magnetohydrodynamic simulations to study the
evolution of a supernova remnant (SNR) in a turbulent neutral atomic
interstellar medium. The media used as background shares characteristics with
the Solar neighbourhood and the SNR has mass and energy similar to those of a
Type Ia object. Our initial conditions consist of dense clouds in a diluted
medium, with the main difference between simulations being the average
magnitude of the magnetic field. We measured amplifications of the magnetic
energy of up to 34$\%$ and we generated synthetic maps that illustrate how the
same object can show different apparent geometries and physical properties when
observed through different lines of sight.
