Mass loss from rotating hot-stars: Inhibition of wind compressed disks by nonradial line-forces

We review the dynamics of radiatively driven mass loss from rapidly rotatin g hot-stars. We first summarize the angular momentum conservation process t hat leads to formation of a Wind Compressed Disk (WCD) when material from a rapidly rotating star is driven gradually outward in the radial direction. We next describe how stellar oblateness and asymmetries in the Sobolev lin e-resonance generally leads to nonradial components of the driving force is a line-driven wind, including an azimuthal spin-down force acting against the sense of the wind rotation, and a latitudinal force away from the equat or. We summarize results from radiation-hydrodynamical simulations showing that these nonradial forces can lead to an effective suppression of the equ atorward flow needed to form a WCD, as well as a modest (similar to 25%) sp in-down of the wind rotation. Furthermore, contrary to previous expectation s that the wind mass flux should be enhanced by the reduced effective gravi ty near the equator, we show here that gravity darkening effects can actual ly lead to a reduced mass loss, and thus lower density, in the wind from th e equatorial region. Finally, we examine the equatorial bistability model, and show that a sufficiently strong jump in wind driving parameters can, in principle, overcome the effect of reduced radiative driving flux, thus sti ll allowing moderate enhancements in density in an equatorial, bistability zone wind.