  We simulate the formation of bipolar planetary nebulae (PNe) through very
short impulsive mass ejection events from binary systems, where the asymptotic
giant branch (AGB) star ejects a mass shell that is accelerated by jets
launched from a compact companion. The acceleration process takes place at very
short distances from the binary system, such that the photon-diffusion time is
long enough to prevent rapid cooling of the shocked jets' material. When the
shocked jets' gas density is lower than the shell density the flow becomes
Rayleigh-Taylor unstable and dense clumps are formed in the flow. At later
times a PN with clumpy lobes that have a linear distance-velocity relation will
be observed. This process might account for the formation of bipolar PNe with
clumpy lobes, such as NGC 6302. The energy radiated during the months to years
duration of such an event will appear as an intermediate-luminosity optical
transient (ILOT)
