We examine the influences of the orbital motion of wide binary progenitors on the structures of the descendent planetary nebulae (PNe). We focus on orbital separations in the range a-30 au to a few x 103 au. When the orbital period is much shorter than the mass-loss episode, the effects are of second order in the ratio of orbital to wind velocity, and are therefore small. Very wide binaries with orbital periods comparable to, or longer than, the mass-loss episodes will cause deviations from axisymmetry. At late times the density enhancement in the equatorial plane may resemble the structure of PNe moving through the ISM, or changes in the wind properties. These structural features may indicate the existence of wide binary systems in the cores of planetary nebulae possessing the features. The results of this paper may be applied to circumstellar matter around more massive stars, such as progenitors of supernovae (SNe), by rescaling the physical properties of the binary orbits and wind velocities.
- Binaries: General-circumstellar matter-stars: Mass-loss-planetary nebulae: General