CC BY-NC-ND 4.0 UnportedMunari, U.Siviero, A.Tamajo, E.Fiaschi, M.Dallaporta, S.Cherini, G.Frigo, A.Castellani, F.Graziani, M.Moretti, S.Tomaselli, S.2020-09-112020-09-112012https://doi.org/10.34657/4274https://oa.tib.eu/renate/handle/123456789/5645We have collected high precision optical photometry of VV8, so far 782 individual observing runs uniformly distributed over the period 2005-2011. This dataset allows us to refine the known long periodicity of VV8 to P = 16.8 yr, with peak-to-valley amplitudes of ΔB = 0.18 and ΔV = 0.14 mag. In addition, we have discovered two new periodicities: 6.431 d (total amplitude Δ = ΔV = ΔI= 0.05 mag) and 1.185 d (ΔB = 0.022, ΔV = 0.018, ΔI = 0.014 mag). These two short periods are reminiscent of the Abell35 phenomena displayed by binary nuclei of planetary nebulae that have gone through a common envelope phase. Twice the 6.431 d period would nicely correspond to the double-peaked light-curve that the G5 III star in VV8 would display if its Roche lobe would be ellipsoidally distorted.enghttps://creativecommons.org/licenses/by-nc-nd/4.0/550Planetary nebulae: Central starStars: Symbiotic binariesArticle