  I propose that at the termination of the common envelope evolution (CEE) the
companion to the giant star might launch jets that have variable directions and
intensities, hence the jets shape the inner zones of the descendant nebula
causing it to lose any type of symmetry. This might account for some of the
chaotic departures from axisymmetric structures in some planetary nebulae. I
base my study on the assumption that at the termination of the CEE the binary
interaction forms a circumbinary thick disk that feeds the companion via an
accretion disk that launches opposite jets. I consider two processes that might
lead to the development of Rayleigh-Taylor instabilities that lead to chaotic
accretion flow on to the companion. The chaotic accretion flow leads to a
variable accretion disk around the companion, hence to variable jets. In the
first process the jets inflate low-density hot bubbles in the inner regions of
the envelope. In the second process the inner boundary of the thick
circumbinary disk, that faces the center, cools by radiation thus leading to a
temperature, and hence also a pressure, increase with radius. The opposite
pressure and density gradients lead to Rayleigh-Taylor instabilities. This
study further underlines the importance of exploring the termination phase of
the CEE to the understanding of the entire CEE and its outcomes.
