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The effects of the stellar rotation and the consequent azimuthal stellar windflow in Parker's [9] hydrodynamic stellar wind model are discussed. Of specialinterest is the emergence of a whole new hydrodynamic physics via a newcritical point in the stellar wind flow, which supersedes the critical point inParker's [9] hydrodynamic model. The effect of the stellar rotation is shown tocause the new critical point to occur lower in the corona, so the stellar windexperiences a stronger afterburner (as in an aircraft jet engine) action in thecorona. For strong rotators, the new critical point is shown to occur at afixed location for a given star, determined only by the basic stellarparameters like the mass M and the angular velocity, the variations in thestellar wind environment notwithstanding. The stellar rotation leads tostronger density fall-off and enhanced acceleration of the stellar wind atlarge distances from the star - this effect materializes even close to thestar, for strong rotators. The stellar rotation causes the physical throatsection of the effective de Laval nozzle associated with the stellar wind flowto become narrower, indicative of an enhanced flow acceleration. Thus, thestellar rotation leads to tenuous and faster stellar wind flows without changein the mass flux, and hence provides an efficient physical mechanism forprotostars and strong rotators to lose their angular momentum quickly.

Effects of Stellar Rotation in Parker's Hydrodynamic Stellar Wind Model: How Protostars and Strong Rotators Lose their Angular Momentum Fast