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We constructed dual abundance photoionization models of SMC N87 alongthe principles laid out by Péquignot et al. (2002) in their modelling of the GalacticPN NGC6153. Recent spectroscopic studies have necessitated this approachif one wants to interpret correctly the faint, heavy element optical recombinationlines (ORLs) seen in the spectra of PNe and H Π regions. The semi-empiricalanalysis of Tsamis et al. (2003, 2004) has shown that in N87 the abundancesof C and O, relative to H, derived from ORLs are a factor of 2–3 larger thanthose derived from collisionally excited lines (CELs). This discrepancy can beexplained by introducing chemical inhomogeneities in the nebula in the form ofhydrogen-de.cient, cold plasma regions.

Chemically Inhomogeneous Photoionization Modelling of the Planetary Nebula SMC N87