  The morphology of planetary nebulae emerging from the common envelope phase
of binary star evolution is investigated. Using initial conditions based on the
numerical results of hydrodynamical simulations of the common envelope phase it
is found that the shapes and sizes of the resulting nebula are very sensitive
to the effective temperature of the remnant core, the mass-loss rate at the
onset of the common envelope phase, and the mass ratio of the binary system.
These parameters are related to the efficiency of the mass ejection after the
spiral-in phase, the stellar evolutionary phase (i.e., RG, AGB or TP-AGB), and
the degree of departure from spherical symmetry in the stellar wind mass loss
process itself respectively. It is found that the shapes are mostly bipolar in
the early phase of evolution, but can quickly transition to elliptical and
barrel-type shapes. Solutions for nested lobes are found where the outer lobes
are usually bipolar and the inner lobes are elliptical, bipolar or barrel-type,
a result due to the flow of the photo-evaporated gas from the equatorial
region. It is found that the lobes can be produced without the need for two
distinct mass ejection events. In all the computations, the bulk of the mass is
concentrated in the orbital or equatorial plane, in the form of a large toroid,
which can be either neutral (early phases) or photoionized (late phases),
depending of the evolutionary state of the system.
