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We have simulated a common envelope interaction of a 0.88-M$_{\odot}$,90-R$_{\odot}$, red giant branch star and a 0.6-M$_{\odot}$, compact companionwith the smoothed particle hydrodynamics code, Phantom, from the beginning ofthe Roche lobe overflow phase to the beginning of the self-regulated inspiral,using three different resolutions. The duration of the Roche lobe overflowphase is resolution dependent and would lengthen with increased resolutionbeyond the $\sim$20 years observed, while the inspiral phase and thepost-common envelope separation are largely independent of resolution. Masstransfer rates through the Lagrangian points drive the orbital evolution duringthe Roche lobe overflow phase, as predicted analytically. The absolute masstransfer rate is resolution dependent, but always within an order of magnitudeof the analytical value. Similarly, the gravitational drag in the simulationsis close to the analytical approximation. This gives us confidence thatsimulations approximate reality. The $L_2$ and $L_3$ outflow observed duringRoche lobe overflow remains bound, forming a circumbinary disk that is largelydisrupted by the common envelope ejection. However, a longer phase of Rochelobe overflow and weaker common envelope ejection typical of a more stablebinary may result in a surviving circumbinary disk. Finally, we examine thedensity distribution resulting from the interaction for simulations thatinclude or omit the phase of Roche lobe overflow. We conclude that the degreeof stability of the Roche lobe phase may modulate the shape of the subsequentplanetary nebula, explaining the wide range of post-common envelope planetarynebula shapes observed.

Extending Common Envelope Simulations from Roche Lobe Overflow to the Nebular Phase