We examine how the characteristics of Supernova remnant (SNR) shocks evolve in a non-uniform
background with a non-isotropic ejection using the MHD code of Athena++. As an example, the
remnant SN1006 is modelled using various scenarios. The turbulent density and magnetic field in
the background interstellar medium (ISM) are assumed to have a Kolmogorov spectrum. Using
the spherical harmonic function 𝑌𝑙,𝑚 (𝜃, 𝜙) as a basis, we model the non-isotropic ejection also by
a Kolmogorov-like spectrum in (l,m). We consider cases where the ejecta speed in one direction
differs significantly from other directions by adding a Gaussian profile to the ejection profile.
Simulation results are compared to cases of an isotropic supernova explosion in both a uniform
and non-uniform background. We find that the morphology of the SNR shock looks noticeably
different at earlier times for different scenarios. In later times, ∼ 1, 000 years, the differences
become smaller. Synthetic synchrotron radiation maps for different scenarios are obtained and
compared to observations.