Surprising Variability of the Planetary Nebula IC 4997 = QV Sge

We present the results of a new epoch of a long-term photometric monitoring of the variable planetary nebula IC~4997. The integral $UBV$ light curves display a continuing brightening of 0.$^{m}15$ in $V$, a slight rise ( 2$ from 1990 to 2019, whereas the [OIII] $\lambda$4363 line had weakened by a factor of 2 comparing to the maximum value observed in 2000. The variation of H$\beta$ absolute intensity in 1960-2019 was shown to be similar to that of [OIII] nebular lines, but of smaller amplitude. The electron density in the outer part of the nebula was estimated from the [SII] and [ClIII] lines. Basing on the data on absolute intensities we propose a possible scenario describing the change of $N_e,T_e$ in 1970-2019. The spectral variability of IC~4997 could be explained by a variation of electron temperature in the nebula caused by not so much the change in ionizing flux from the central star as the variable stellar wind and related processes. The photometric and spectral changes observed for IC~4997 in 1960-2019 may be interpreted as an observable consequence of a single episode of enhanced mass loss from the variable central star.