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We explore the effects of photodissociation at the stages of post-asymptoticgiant branch stars to find a mechanism able to produce multi-polar shapes. Weperform two-dimensional gasdynamical simulations to model the effects ofphotodissociation in proto-planetary nebulae. We find that post-asymptoticgiant branch stars with 7,000 K or hotter are able to photodissociate a largeamount of the circumstellar gas. We compute several solutions for nebulae withlow-velocity multi-lobes. We find that the early expansion of a dissociationfront is crucial to understand the number of lobes in proto-planetary nebulae.A dynamical instability appears when cooling is included in the swept-upmolecular shell. This instability is similar to the one found inphotoionization fronts, and it is associated with the thin-shell Vishniacinstability. The dissociation front exacerbates the growth of the thin-shellinstability, creating a fast fragmentation in shells expanding into media withpower-law density distributions such as r^-2.

Photodissociation in proto-planetary nebulae. Hydrodynamical simulations and solutions for low-velocity multi-lobes