assess how well a model originally developed for large-scale coronal jets PAD09 can explain the properties of jet-like features appearing in the lower layers of the solar atmosphere.

The 3D MHD model of PAD09 was developed to explain the helical properties of coronal jets and was found to properly match numerous features of a helical jet observed with STEREO [@Patsourakos08]. Subsequently, this model has been developed in a series of parametric studies that have explored different aspects of the generation of jets, such as the role of reconnection [@Rachmeler10], the occurrence of homologous jets [@Pariat10 hereafter PAD10], the influence of the photospheric and coronal magnetic geometry (PDD15), the generation of straight and helical jets (PAD10, PDD15), their propagation in spherical geometry from the gravitationally stratified solar corona into the solar wind [@Karpen16]. and jets confined by closed coronal loops [@Wyper16; @Wyper16b].

A critical parameter that defines the different environments of the solar atmosphere is the plasma $\beta$, defined as the ratio of the gas pressure to the magnetic pressure. It is well established that in the highly magnetised corona, the dynamics of the plasma overall are dominated by the Lorentz force $(\beta <<1)$, whereas the gas pressure dominates within the 