  We discuss the formation of planetary nebulae (PNe) having a pair of lobes,
or multi-lobes, in their inner region surrounded by an elliptical or spherical
shell or halo. We suggest that most of these PNe are formed by wide binary
systems, with final orbital periods in the range of 40-10,000 years, such that
there is no strong tidal interaction. The outer more spherical structure is
formed from the early asymptotic giant branch (AGB) wind. Toward the end of the
AGB the mass loss rate increases, and wind velocity possibly decreases, making
the conditions for the formation of an accretion disk around the wide
companion, more favorable. We assume that the accreting companion blows jets or
a collimated fast wind (CFW), which lead to the formation of a pair of lobes in
the inner region. In cases of a precessing accretion disk, a multi-lobes
structure can be formed. We conduct a population synthesis study of such
systems, and find that overall 5-20 percents of all PNe are formed by such
binary systems. We also estimate that 20-40 percents of these systems possess
observable departure from axisymmetry, e.g., the central star is not in the
center of the nebula.
