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This analysis models radiatively driven winds in stars, revealing key singular points affected by radiation terms.
A model of a radiatively driven, magnetohydrodynamic wind flow confined in the equatorial plane of the star is formulated and the basic eqations are preliminalily analyzed. It is shown that major singular points of the basic equations are slow magnetosonic, the Alfvenic and fast magnetosonic points. The two magnetosonic points are modified by the radiation terms. When the star does not rotate at a slower velocity than at its break-up velocity, the slow magnetosonic point never exists outside the star.
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Yasumichi Saito (1990) studied this question.
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