Common-envelope shaping of planetary nebulae – IV. From protoplanetary to planetary nebula

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