Panels a and b: number density in cm⁻³ and the magnetic field lines of simulation X-b5 in the initial configuration and after an evolution of 158 inner orbits at r = r₀ (≈ 1.8 orbits at 20 au), where a strong wind emerges. A slightly asymmetric flow forms in the inner region. Panels c and d: ionization fraction x_e in the disk. The snapshot after 158 orbits at r = r₀ visualizes the reduced ionization fraction due to the thick wind flow.