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Optical spectra of the 2006 outburst of RS Ophiuchi beginning one day afterdiscovery to over a year after the outburst are presented here. The spectralevolution is found to be similar to that in previous outbursts. The early phasespectra are dominated by hydrogen and helium (I & II) lines. Coronal andnebular lines appear in the later phases. Emission line widths are found tonarrow with time, which is interpreted as a shock expanding into the red giantwind. Using the photoionisation code CLOUDY, spectra at nine epochs spanning 14months after the outburst peak, thus covering a broad range of ionisation andexcitation levels in the ejecta, are modelled. The best-fit model parametersindicate the presence of a hot white dwarf source with a roughly constantluminosity of 1.26 x 10^{37} erg/s. During first three months, the abundances(by number) of He, N, O, Ne, Ar, Fe, Ca, S and Ni are found above solarabundances; abundances of these elements decreased in the later phase. Alsopresented are spectra obtained during quiescence. Photoionisation model of thequiescence spectrum indicates the presence of a low luminosity accretion disk.The helium abundance is found to be subsolar at quiescence.

Optical spectroscopy of the recurrent nova RS Ophiuchi - from the outburst of 2006 to quiescence