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Planetary nebulae(PNe) represent the end stage of low-to-intermediate stars, with most of them having hydrogen-rich central stars. About 15% of them exhibit Wolf-Rayet phenomena ([WR] stars) with hydrogen-deficient, helium and carbon-rich atmospheres. These stars are very hot and luminous, with strong and dense stellar winds. Infrared properties reveal that [WR] PNe exhibit distinctive characteristics compared to non-[WR] PNe, pointing to their different evolutionary scenarios. Detailed radiative transfer modelling is required to unveil their intricate thermal and photo-ionization structures and to understand their unique evolutionary paths compared with normal ones. Our present study incorporates UV and optical medium-resolution spectroscopic data with IRAS photometric flux, absolute Hꞵ flux and the size of the emitting region to constrain the 1D Dusty photo-ionization model effectively. This investigation aims to elucidate the underlying physical conditions of both gas and dust components and to determine the initial mass of the progenitor star. We present here a case study for [WR] PN IC 2003. Notably, the presence of abundant small grains in [WR] PNe amplifies photoelectric heating, impacting nebular emission lines and excitation equilibrium balance. By considering various small grain size distributions in our model, we address the significance of grain heating in the nebula and also identify the most appropriate grain size distribution. Our model revealed significant differences in abundances and central star parameters compared to empirical values and prior studies. The mass of the progenitor was determined to be 3.2 M.BGS OFFICE