  I propose a scenario for the formation of double-ring systems, as observed in
some planetary nebulae and in the outer rings of SN 1987A. In this scenario,
two jets, one jet on each side of the equatorial plane, expand into a thin,
dense shell. Such a flow is expected in binary systems where the mass-losing
primary undergoes an impulsive mass loss episode which forms a thin, dense
shell. I assume that a small fraction of that mass is accreted onto a companion
which blows the jets. Each jet accelerates shell's material it hits sideways,
forming a higher density ring. Using several simplifying assumptions, I derive
an expression for the radius of the ring, which depends relatively weakly on
the jets and impulsive mass loss episode properties. This shows that such a
scenario is feasible. If there are several such impulsive mass loss episodes,
more double rings will be formed, as observed in the planetary nebulae MyCn 18
(the Hourglass nebula). Because of the binary interaction and orbital motion,
the double-ring system is displaced from the symmetry axis of the main nebula,
as observed.
