  A large number of massive stars are known to rotate, resulting in significant
distortion and variation in surface temperature from the pole to the equator.
Radiatively driven mass loss is temperature dependent, so rapid rotation
produces variation in 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 investigate the two dimensional
effects of rotation on radiatively driven mass loss and the associated loss of
angular momentum in ZAMS models with solar metallicity. Using 2D stellar
models, which give the variation in surface parameters as a function of
co-latitude, 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 co-latitude. We find that the
mass loss rate decreases as the rotation rate increases for models at 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.
