  Young stellar objects/planetary nebula outflow anisotropies usually involve
wind-wind interactions and magnetic collimation, but detailed structures of
wind and magnetic fields inside collimation region remain undetermined. We
numerically investigated its laboratory counterpart, based on poloidal field
collimation in magnetocentrifugal launching model. Our analog consist of fast
wind: Aluminum plasma generated by laser and magnetized ambient: molecular
Helium and B=5-60 Tesla embedded field. Elevating magnetic field strength or
decreasing gas density can alter expansion morphology, from sphere to prolonged
cavity and ultimately to collimated jet. Outflow patterns can be quantitatively
predicted based on the knowledge of its surroundings through a set of external
Mach numbers. We conclude that such mixed gas and magnetic field dynamics are
consistent with astronomical observations of protostars and planetary nebulae
in certain evolution stages, and here provide a scalable framework allowing
fitting of flow-field structures in astronomical unresolved regions by assuming
their possible geometries on a repeatable laboratory platform.
