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The standard, or fast, solutions of m-CAK line-driven wind theory cannotaccount for slowly outflowing disks like the ones that surround Be stars. Ithas been previously shown that there exists another family of solutions --- the$\Omega$-slow solutions --- that is characterized by much slower terminalvelocities and higher mass-loss rates. We have solved the one-dimensional m-CAKhydrodynamical equation of rotating radiation-driven winds for this lattersolution, starting from standard values of the line force parameters ($\alpha$,$k$, and $\delta$), and then systematically varying the values of $\alpha$ and$k$. Terminal velocities and mass-loss rates that are in good agreement withthose found in Be stars are obtained from the solutions with lower $\alpha$ andhigher $k$ values. Furthermore, the equatorial densities of such solutions arecomparable to those that are typically assumed in ad hoc models. For very highvalues of $k$, we find that the wind solutions exhibit a new kind of behavior.

Line-Driven Winds Revisited in the Context of Be Stars: $\Omega$-slow Solutions with High $k$ Values