Abstract:
We report dusty photo-ionization models for two Planetary Nebulae NGC 2452 and IC 2003, which have [WR] type central stars,
using 1D photo-ionization code Cloudy17.02. We used the medium resolution optical spectra and archival IRAS photometry to con-
strain our models. The physical size of the ionized nebula derived using accurate distance measurements and absolute Hb flux available
in the literature were used as additional constrains. We examine the importance of photo-electric heating and found that models with and
without considering photo-electric heating do not make significant difference for both PNe for the MRN grain size distribution consid-
ered in this study. We derive the nebular elemental abundances of these PNe by the empirical method as well as by making dusty photo-
ionization models. The values of N/O ratios for both PNe obtained from our models are lower than their respective values arrived using
empirical methods. The central stars are assumed to be black bodies and the photospheric temperatures derived respectively for NGC
2452 and IC 2003 from their best fit models are 182 kK and 155 kK and their respective luminosities are 630L and 1015L . We propose
that both the PNe were resulted from low-mass progenitors of mass 62.8 M⊙.
