Latitudinal Dependence of Radiatively Driven Mass Loss from Rapidly Rotating Hot-Stars
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We investigate the latitudinal variation of radiatively driven mass loss from rapidly rotating hot-stars. Previous analyses have assumed a uniformly bright stellar surface and concluded that the wind mass flux and density should increase with the increased centrifugal force toward the wind equator. In contrast, we show here that a gravity darkening in which the surface radiation flux scales with the effective (centrifugally reduced) gravity leads to a dramatically different wind morphology, with the strongest mass loss now occurring toward the relatively bright poles. We also review recent work that indicates nonradial (poleward) components of the line-driving force in such rotating winds can effectively inhibit the equatorward wind deflection needed to form an equatorial wind-compressed disk. 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 still allowing moderate enhancements in density in an equatorial, bistability zone wind.
KeywordsMass Flux Stellar Surface Angular Momentum Conservation Effective Gravity Equatorward Flow
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