Top panel A): gas density in g/cm³ (right) and dust grain particle density in cm^-3 (left) for simulation A after 1.37 × 10⁵ years; basic model. The bow shock is smooth, but at the contact discontinuity both Rayleigh-Taylor and Kelvin-Helmholtz instabilities are visible. Bottom panel B): similar to top panel, but for simulation B after 5.0 × 10⁴ years; high Ṁ. The instabilities are now primarily of the Rayleigh-Taylor type. Due to the stronger wind the bow shock lies further from the star.