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 \times 10 ^ { 3 } G ) can roughly reproduce the latitude-dependent wind required to form the peculiar periphery of Tycho ’ s SNR .