SIMBAD references

A large number of massive stars are known to rotate rapidly, resulting in a significant distortion and variation in surface temperature from the pole to the equator. Radiatively driven mass-loss is temperature-dependent, so rapid rotation produces a variation in the mass-loss and angular momentum loss rates across the surface of the star, which is expected to affect the evolution of rapidly rotating massive stars. In this work, we use zero-age main-sequence (ZAMS) stellar models to investigate the two-dimensional effects of rotation on stellar mass-loss, using two common prescriptions for radiatively driven mass-loss. The associated loss of angular momentum from these models is also considered. Using 2D stellar models, which give the variation in surface parameters as a function of colatitude, we implement two different mass-loss prescriptions describing radiatively driven mass-loss. We find a significant variation in mass-loss rates and angular momentum loss as a function of colatitude. We find that the mass-loss rate decreases as the rotation rate increases for models with a constant initial mass, and derive scaling relations based on these models. When comparing 2D to 1D mass-loss rates, we find that although the total angle integrated mass-loss does not differ significantly, the 2D models predict less mass-loss from the equator and more mass-loss from the pole than the 1D predictions using von Zeipel's law. As a result, rotating models lose less angular momentum in 2D than in 1D, which will change the subsequent evolution of the star. The evolution of these models will be investigated in future work.