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In this paper we focus on the construction of stellar outflow models emergingfrom a polar coronal hole-type region surrounded by a magnetosphere in theequatorial regions during phases of quiescent accretion. The models are basedon initial analytical solutions. We adopt a meridionally self-similar solutionof the time-independent and axisymmetric MHD equations which describeseffectively a jet originating from the corona of a star. We modifyappropriately this solution in order to incorporate a physically consistentstellar magnetosphere. We find that the closed fieldline region may exhibitdifferent behaviour depending on the associated boundary conditions and thedistribution of the heat flux. However, the stellar jet in all finalequilibrium states is very similar to the analytical one prescribed in theinitial conditions. When the initial net heat flux is maintained, themagnetosphere takes the form of a dynamical helmet streamer with a quasi steadystate slow magnetospheric wind. With no heat flux, a small dead zone formsaround the equator, surrounded by a weak streamer, source of a low mass fluxmagnetospheric ejection. An equilibrium with no streamer and a helmet shapeddead zone is found when the coronal hole is larger and extends up to a reducedclosed fieldline static zone. The study demonstrates the robustness ofself-similar solutions and their ability to provide quasi-steady jetsimulations with realistic boundaries and surrounded by equatorialmagnetospheres.

Modelling stellar jets with magnetospheres using as initial states analytical MHD solutions