Abstract
Ring Planetary Nebulae associated with secondary structures or not, are considered as objects belonging to the typical «Butterfly Nebulae» class. They are seen at different inclination angles with respect to the plane of the sky, as pointed out by Minkowski and Osterbrock (1960). Our monochromatic observations made at both ESO (Chile) and Observatoire de Haute-Provence (France) all favour the geometrical structure assuming two bubbles located on both sides of a denser toroid. In order to take into account the fact that Ring Planetary Nebulae are seen in different evolutionary stages, the Champagne Model is proposed following the Tenorio-Taggle effect (1979) coupled with the rotation of the nucleus (Louise, 1973).
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