  AG Draconis is a bright symbiotic binary consisting of a white dwarf and a
pulsating cool giant. Moreover, it is the most intense X-ray source among
symbiotic stars, and one of the best representatives of the super-soft X-ray
objects. The system undergoes characteristic symbiotic activity with
alternating quiescent and active stages. The active ones consist of several
outbursts repeating at about a one-year interval. The recent activity stage of
AG Dra began with the weak pre-outburst in 2015 followed by a more prominent
outburst in 2016. According to photometric and some spectroscopic observations,
both brightenings belong to the minor (hot) outbursts of AG Dra. Such behavior
of the active stage is quite unusual because more often, the activity of AG Dra
starts with a major (cool) outburst. Moreover, the behavior of Raman scattered
OVI lines at {\lambda} 6825 {\AA} and {\lambda} 7082 {\AA} suggest that the
minor outburst of AG Dra in April 2016 has the characteristics of both the hot
and cool outbursts. Based on the above, an open question is the next evolution
of activity of the symbiotic binary AG Dra in 2017 and beyond.

Solar and Stellar Astrophysics