are marginally detected while in the spectra between +60d and +99d they are prominent. We investigate the temporal change of EW of a relatively less blended  $\lambda$4924 and from the spectra normalized to the  peak value, we found that at an EW $\sim$ 0.67 Å at +14d, increased to 17.45 Å at +54d and to 26.53 Å in the +99d spectrum. Later on, the EW decreased to 19.07 Å in the +118d spectrum and finally reaches to 18.27 Å in the +143d spectrum. This rapid fall in the EW of inner metal-rich shells plausibly indicates a decrease in the opacity of the SN inner ejecta.

Traces of the  $\lambda$5876 line are also seen in the +7d spectrum (Figure \[fig:vel\_line\]). The ratio of EWs between  and  for this spectrum is EW()/EW() $\sim 1.99$. In the +14d spectrum, this ratio has increased to 5.36. The steep decrement in EW of  seems to be due to a quick recombination of  ions as a result of the rapid fall in temperature of the constantly rarefying ejecta. From +54d, the emerging P-Cygni feature of  D becomes prominent. This feature seems to be a perfect P-Cygni throughout our entire spectral sequence. It simply indicates an uniform 