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While analysing the images of the IPHAS H$\alpha$ survey, we noticed that thecentral star of the candidate planetary nebula IPHASXJ211420.0+434136 (alsonamed Ou5) was clearly variable. This is generally considered as an indicationof binarity. To confirm it, we performed a photometric monitoring of thecentral star, and obtained images and spectra of the nebula.  The nebular spectrum confirms that IPHASXJ211420.0+434136 is a planetarynebula of moderately high excitation. It has a remarkable morphology with twonested pairs of bipolar lobes, and other unusual features. The light curve ofthe central star reveals that it is an eclipsing binary system with an orbitalperiod of 8.74 hours. It also displays a strong irradiation effect with anamplitude of 1.5~mag.  The presence of multiple bipolar outflows adds constraints to the formationof these nebulae, suggesting the occurrence of discrete ejection events during,or immediately before, the common-envelope phase.  IPHASXJ211420.0+434136 also adds evidence to the hypothesis that asignificant fraction of planetary nebulae with close binary central stars havea peculiar nebular chemistry and a relatively low nebular mass. This may pointto low-mass, low-metallicity progenitors, with additional effects related tothe binary evolution. We also suggest that these objects may be relevant tounderstand the abundance discrepancy problem in planetary nebulae.

The planetary nebula IPHASXJ211420.0+434136 (Ou5): insights into common-envelope dynamical and chemical evolution