that different photospheric magnetic distributions strongly affect the generation of the [[straight jet]{}]{}. From the first parametric studies presented in PDD15 we showed that a preceding reconnection-driven straight jet profoundly influences the onset of the succeeding [[helical jet]{}]{}. The third parametric study reported here will extend these results by showing that the actual occurrence of a [[straight jet]{}]{}is not essential, the early existence of intense reconnection is the key element that affects the trigger of the helical jet.

The parametric study presented here, however, goes further than merely confirming the results of PDD15. We present a completely new analysis of the underlying physical mechanism that accelerates the plasma in our model (Sect. \[sec:Betadriver\]). By varying $\beta$, we also show the original result that the morphology of the jet is strongly influenced by this parameter, a finding that was not expected from our previous simulations.

Model description {#sec:Model}
=================

The simulations presented here extend the work presented in @Pariat15a [PDD15]. In the simulations, we consider the equations of ideal magneto–hydrodynamics (MHD) for a monofluid coronal plasma of uniform density and temperature. The simulations were performed with the [*A*]{}daptively [*R*]{}efined [*M*]{}agnetohydrodynamic [*S*]{}olver ([*ARMS*]{}), whose Flux-Corrected Transport algorithms are extensions of those derived 