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We present 2D hydrodynamical simulations of the transition of aproto-planetary nebula to a planetary nebula for central stars in binarysystems that have undergone a common envelope event. After 1,000 yr ofmagnetically driven dynamics (proto-planetary nebula phase), a line-drivenstellar wind is introduced into the computational domain and the expansion ofthe nebula is simulated for another 10,000 yr, including the effects of stellarphotoionization. In this study we consider central stars with main sequence(final) masses of 1 (0.569) and 2.5 (0.677) \Mo, together with a 0.6 \Mo ma insequence companion. Extremely bipolar, narrow-waisted proto-planetary nebulaeresult in bipolar planetary nebulae, while the rest of the shapes mainly evolveinto elliptical planetary nebulae. The initial magnetic field's effects on thecollimated structures, such as jets, tend to disappear in most of the cases,leaving behind the remnants of those features in only a few cases. Equatorialzones fragmented mainly by photoionization ( 1 \Mo progenitors), result in``necklace'' structures made of cometary clumps aligned with the radiationfield. On the other hand, fragmentation by photoionization and shocked wind (2.5 \Mo progenitors) give rise to the formation of multiple clumps in thelatitudinal direction, which remain within the lobes, close to the center,which are immersed and surrounded by hot shocked gas, not necessarily alignedwith the radiation field. These results reveal that the fragmentation processhas a dependence on the stellar mass progenitor. This fragmentation is madepossible by the distribution of gas in the previous post-common envelopeproto-planetary nebula as sculpted by the action of the jets.

Common Envelope Shaping of Planetary Nebulae. IV. From Proto-planetary to Planetary Nebula