In order to explain the observed rotation in bipolar outflow (e.g. Zapata et al. 2015), we present a time dependent model of the interaction between a stellar wind and an accretion flow. We consider that the bipolar outflow is a thin shell formed by the shock between an isotropic stellar wind and a rotating cloud in gravitational collapse, also we assume symmetry with respect
to the cloud’s rotational axis. The hydrodynamics equations are integrated and obtained a set of partial differential equations in τ, r, θ, and φ, these equations are solved numerically and we find the shape of the shell, the velocity field, surface density and angular momentum rate of the material into the shell, in addition, we obtain the radial velocity along the line of sight in order to compare the theoretical results with the observational data.