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We perform photoionization modeling of the dusty nova V1280 Scorpii (V1280Sco) with an aim to study the changes in the physical and chemical parameters.We model pre and post dust phase, optical and near-Infrared (NIR), spectrausing the photoionization code \textsc{cloudy}, v.17.02, considering atwo-component (low density and high density region) model. From the best-fitmodel, we find that the temperature and luminosity of the central ionizingsource in the pre-dust phase are in the range 1.32 - 1.50 $\times 10^4$ K and2.95 - 3.16 $\times 10^{36}$ ergs$^{-1}$, respectively, which increase to 1.58- 1.62 $\times 10^4$ K and 3.23 - 3.31 $\times 10^{36}$ ergs$^{-1}$,respectively, in the post-dust phase. It is found that a very high hydrogendensity ($\sim 10^{13} - 10^{14}$ cm$^{-3}$) is required for the generation ofspectra properly. Dust condensation conditions are achieved at high ejectadensity ($\sim 3.16 \times 10^{8}$cm$^{-3}$) and low temperature ($\sim$2000 K)in the outer region of the ejecta. It is found that a mixture of small (0.005 -0.25$\mu$m) amorphous carbon dust grains and large (0.03 - 3.0$\mu$m)astrophysical silicate dust grains iis present n the ejecta in the post-dustphase. Our model yields very high elemental abundance values as C/H = 13.5 -20, N/H = 250, O/H = 27 - 35, by number, relative to solar in the ejecta,during the pre-dust phase, which decrease in the post-dust phase.

Photoionization modeling of the dusty nova V1280 Scorpii