The radiatively driven winds of intermediate mass main-sequence stars (4-9M_O corresponding to spectral types later than B2-3) have low mass-loss rates. These winds have been shown to be susceptible to ion stripping - where the heavy element ions (responsible for intercepting the star's UV photons and hence driving the flow) decouple from the rest of the wind. Post-decoupling, the flow receives no further acceleration and its dynamics are determined by gravity and gas pressure. The wind can be either unbound or still bound to the star depending on the velocity of the wind at decoupling.

The flows of both bound and unbound winds created by decoupling are discussed with the aid of 1D and 2D numerical hydrodynamic simulations.