  We simulate the evolutions of the stellar wind and the supernova remnant
(SNR) originating from a runaway massive star in an uniform Galactic
environment based on the three-dimensional magnetohydrodynamics models. Taking
the stellar wind into consideration, we can explain the radio morphologies of
many supernova remnants. The directions of the kinematic velocity of the
progenitor, the magnetic field and the line of sight are the most important
factors influencing the morphologies. If the velocity is perpendicular to the
magnetic field, the simulation will give us two different unilateral SNRs and a
bilateral symmetric SNR. If the velocity is parallel to the magnetic field, we
can obtain a bilateral asymmetric SNR and a quasi-circular SNR. Our simulations
show the stellar wind plays a key role in the radio evolution of a SNR, which
implies the Galactic global density and magnetic field distribution play a
secondary role in shaping a SNR.
