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Most stars form in binaries, and both stars may grow by accreting materialfrom a circumbinary disc onto their personal discs. We suspect that in manycases a wide molecular wind will envelope a collimated atomic jet emanatingfrom close to an orbiting young star. This so-called Circumbinary Scenario isexplored here in order to find common identifiable properties. The dynamicalset up is studied with three dimensional simulations with chemistry and coolingincluded. We extract the properties on scales of order 100\,AU and compare tothe Co-Orbital Scenario in which the wind and jet sources are in orbit.  We find that the rapid orbital motion generates a wide ionised sheath aroundthe jet core with a large opening angle at the base. This is independent of thepresence of the surrounding molecular outflow. However, the atomic jet isrecollimated beyond ~ 55 AU when the molecular outflow restricts the motion ofthe ambient medium which, in turn, confines the jet. These physical propertiesare relayed to the optical H-alpha imaging, providing a means of distinguishingbetween models. The high excitation sheath and recollimation region can beexplored on these scales through the next generation of instruments. However,in general, the amount and location of the ionised material, whether in theknots or the sheath, will depend on several parameters including the orbitalperiod, axis alignment and pulse amplitude.

The nature of a primary jet within a circumbinary disc outflow in a young stellar system