The linearized equations governing first-order deviations from the critical, transonic solar-wind flow are examined in special cases. The imposition of a boundary condition corresponding to solar rotation yields the result that the angular momentum of a fluid element is conserved as the element is convected outward with the solar wind. It is demonstrated that, in the domain of existence of the solar wind, coronal self-gravitational attraction is exceedingly small relative to the forces of solar gravity and kinetic pressure. The original neglect of both solar rotation and coronal self-attraction is justified. A general expression for the interplanetary magnetic field, as drawn out from the rotating Sun by a radial plasma flow modified transversely by rotation, is derived. It is demonstrated that, in the region of maximum acceleration, the transverse magnetic force is comparable in magnitude to the zero-order bydrodynamic forces originally incorporated into the model. The desirability of an explicitly hydromagnetic theory of the solar wind is indicated.