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The halo symbiotic star AG Dra has been monitored spectroscopically at the Tartu Observatory, Estonia, from September 1997 to March 2003. Altogether 189 spectra are used in the present paper. In addition, photometric UBVri observations at the Piwnice Observatory, Poland, from March 1996 to May 2003 are presented. Equivalent widths (${\it EW}$) of the strongest emission lines (H α , H β , $\ion{He}{ii}$ λ 4686, $\ion{O}{vi}$ Raman scattered λ 6825) appear to be strongly variable, and in general, correlate with the U brightness of the star. No apparent correlation with the orbital motion of the binary system was found, except for H β in the quiescent state. At the same time, there is a clear convergence of the high values of ${\it EW}$ to certain phases according to the shorter photometric period (378.5 days) proposed by Bastian (1998) and the pulsational period of the cool giant (355.27 days) by Galis et al. (1999). Higher resolution spectra show variability of the H α profiles, with weak absorption component on the blue wing of the line around photometric minimum if the star is in quiescent state. The significant role of the cool giant in the activity of AG Dra is discussed.

Emission lines in the spectrum of the symbiotic star AG Draconis from 1997 to 2003