  We run three-dimensional numerical simulations for the accretion flow around
the white dwarf (WD) in the progenitor system of Tycho's supernova (SN). The
mass of the WD, mass of the companion star, and the orbital period are set to
be 1$M_{\odot}$, 1.6$M_{\odot}$, and 0.794 day, respectively, based on
theoretical and observational researches of Tycho's SN remnant (SNR). We find
that when the magnetic field in the accreted material is negligible, outflowing
wind is concentrated near the equatorial plane. When the magnetic field has
energy equipartition with internal energy, polar wind is comparable with the
equatorial wind. A carefully chosen magnetic field between the above two cases
($B=5.44\times10^3 \rm{G}$) can roughly reproduce the latitude-dependent wind
required to form the peculiar periphery of Tycho's SNR.
