Dust-driven stellar winds in stellar evolution models

Mass loss from stars during their evolution in the HR-diagram is an essential ingredient in stellar evolution models. Mass loss on the AGB is of particular interest when dust production is included in the model, since it is well established that the winds of AGB stars are largely dust driven. For practical reasons, the wind models adopted in stellar evolution codes are relatively simplistic: the actual mass-loss rate is prescribed and net effect of thermal gas pressure is usually not taken into account. In this talk I will discuss how wind these models can be improved without turning them into inhibiting computational challenges. I will also discuss (or speculate about) the effects such an improved wind model can have on the resultant dust yields for AGB stars.