a wide variety of conditions in the solar atmosphere. The tables presented in Appendix \[An:Scaling\] present various possible physical scalings that correspond to our different cases. The simulations using different values of $\beta$ allow us more particularly to determine the dynamics of jets occurring in the different layers of the solar atmosphere. Table \[Tab:Scaling\] presents one set of dimensional quantities that corresponds to different layers of the solar atmosphere for each run. The $\beta=0.025$ and $\beta=0.0025$ runs correspond to corona-like conditions, whereas the transition region would be typically represented with $\beta=0.25$. The $\beta=1$ run is applicable to some aspects of photosphere/chromosphere-like conditions. This correspondence is suggestive, but not definitive, since the chromosphere is a layer with strong density stratification while our simulations assume uniform ambient density. Due to the non-dimensional nature of the MHD system solved here, different $\beta$ simulations can actually correspond to a wide range of parameters. As is shown in the Appendix \[An:Scaling\], a given $\beta$ simulation can apply to different layers for different values of the magnetic field, $B_0$. The layer correspondence in Table \[Tab:Scaling\] is only one possibility.

Note that our simulations focus on calculating the magnetically-driven dynamics of solar jets and not on the 