  We present a comprehensive study of the Magellanic Cloud planetary nebula SMP
61 and of its nucleus, a Wolf-Rayet type star classified [WC 5-6]. We have
performed a detailed spectral analysis of the central star, using the Potsdam
code for expanding atmospheres in non-LTE. The fluxes from the model stellar
atmosphere were used to compute photoionization models of the nebula. All the
available observations, within their error bars, were used to constrain these
models. We find that the ionizing fluxes predicted by the stellar model are
basically consistent with the fluxes needed by the photoionization model to
reproduce the nebular emission, within the error margins. However, there are
indications that the stellar model overestimates the number and hardness of
Lyman continuum photons. The photoionization models imply a clumped density
structure of the nebular material. The observed CIII] 1909/CII 4267 line ratio
implies the existence of carbon-rich clumps in the nebula. Such clumps are
likely produced by stellar wind ejecta, possibly mixed with the nebular
material. We discuss our results with regard to the stellar and nebular
post-AGB evolution.
