  Most radiatively-driven massive star winds can be modelled with m-CAK theory
resulting in so called fast solution. However, those most rapidly rotating
among them, especially when the stellar rotational speed is higher than $\sim
75\%$ of the critical rotational speed, can adopt a different solution called
$\Omega$-slow solution characterized by a dense and slow wind. Here, in this
work we study the transition region of the solutions where the fast solution
changes to the $\Omega$-slow. Using both time-steady and time-dependent
numerical codes, we study this transition region for different equatorial
models of B-type stars. In all the cases, at certain range of rotational
speeds, we found a region where the fast and $\Omega$-slow solution can
co-exist. We find that the type of solution obtained in this co-existence
region depends heavily on the initial conditions of our models. We also test
the stability of the solutions within the co-existence region by performing
base density perturbations in the wind. We find that under certain conditions,
the fast solution can switch to a $\Omega$-slow solution, or vice versa. Such
solution switching may be a possible contributor of material injected into the
circumstellar environment of Be stars, without requiring rotational speeds near
critical values.
