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We present the evolution of the optical spectra of the 2021 outburst of RSOphiuchi (RS Oph) over about a month after the outburst. The spectral evolutionis similar to the previous outbursts. Early spectra show prominent P Cygniprofiles of hydrogen Balmer, \ion{Fe}{ii}, and \ion{He}{i} lines. The emissionlines were very broad during the initial days, which later became narrower andsharper as the nova evolved. This is interpreted as the expanding shockedmaterial into the winds of the red giant companion. We find that the novaejecta expanded freely for $\sim 4$ days, and afterward, the shock velocitydecreased monotonically with time as $v\propto t^{-0.6}$. The physical andchemical parameters associated with the system are derived using thephotoionization code \textsc{cloudy}. The best-fit \textsc{cloudy} model showsthe presence of a hot central white dwarf source with a roughly constantluminosity of $\sim$1.00 $\times$ 10$^{37}$ erg s$^{-1}$. The best-fitphotoionization models yield absolute abundance values by number, relative tosolar of He/H $\sim 1.4 - 1.9$, N/H = $70 - 95$, O/H = $0.60 - 2.60$, and Fe/H$\sim 1.0 - 1.9$ for the ejecta during the first month after the outburst.Nitrogen is found to be heavily overabundant in the ejecta. The ejectedhydrogen shell mass of the system is estimated to be in the range of $3.54 -3.83 \times 10^{-6} M_{\odot}$. The 3D morpho-kinematic modelling shows abipolar morphology and an inclination angle of $i=30^{\circ}$ for the RS Ophbinary system.

Study of 2021 outburst of the recurrent nova RS Ophiuchi: Photoionization and morpho-kinematic modelling