Abstract
Abstract The mass boundary between progenitors of white dwarfs and neutron stars is discussed. We propose obtaining the upper mass limit of WD progenitors from PNe in open clusters. The maximum mass on the main sequence for the OC member stars should be a good estimate of the WD progenitor star's mass in view of the negligible lifetime of PNe. This is a direct and more reliable way for the estimation of the mass boundary between progenitors of WDs and NSs, not having the uncertainties in the progenitor masses found by studying WDs in OCs. Observational and theoretical studies indicate preliminary values about 6–8M ⊙ for the mass boundary between WDs and NSs. PN-OC associations are also necessary to study the connections between masses, chemical abundances and other properties of the PNe, their nuclear stars and the progenitors of these objects on the main sequence. We discuss the association of PNe with OCs and globular clusters. One new association of a PN with GC is found (GC M 15 and PN PK 65–27.2).
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