an [[straight jet]{}]{}. In the high-$\beta$ regime, reconnection may more efficiently produce high-density upflows, while at lower $\beta$, although more magnetic energy is released by reconnection, this energy does not drive high-density plasma flows.

A possible physical origin of this result may be related to our assumed initial conditions. Note that the initial state has a static, uniform density and temperature plasma and a potential magnetic field. Consequently, if interchange reconnection were to occur very easily, for example as soon as the photospheric driving is turned on, no straight jet would be observed, because the closed plasma released by the reconnection would have identical properties to the open. Furthermore, the nonlinear Alfvén wave flux produced by the reconnection would be minimal. In order for the interchange reconnection to produce a large effect, the closed flux must undergo a substantial deformation with a large current sheet built up at the deformed null and a compression of the closed plasma against the dome-like separatrix. This result re-emphasizes the point raised above on the critical importance of the effective Lundquist number of the simulation. We find that, for very low plasma $\beta$, interchange reconnection begins so easily that the released closed plasma is 