  IC\,4997 is a planetary nebula well known by its variability. We present
high-resolution spectra of IC\,4997 obtained in 1993, 2019, and 2020 that
reveal changes in the H$\alpha$ and [N\,{\sc ii}] emission line profiles, which
had never been reported for this object. The H$\alpha$ P\,Cygni emission
profile observed in 1993 changed to a single-peaked profile in 2019--2020,
implying that the stellar wind has largely weakened. The very broad H$\alpha$
emission wings narrowed by a factor of $\sim$2 between 1993 and 2019--2020,
indicating that the efficiency of the Rayleigh--Raman scattering has noticeably
decreased. A high-velocity [N\,{\sc ii}] nebular component detected in 1993 is
missing in 2019 and 2020, probably due to a decrease in its electron density. A
correlation exists between the strength of the stellar wind and the episodic
($\sim$50--60\,yr) variation in the [O\,{\sc iii}]$\lambda$4363/H$\gamma$ line
intensity ratio, suggesting that an episodic, smoothly variable stellar wind is
the main cause of the variability of IC\,4997. Monitoring of that intensity
ratio and of the H$\alpha$ emission line profile in the coming years and new
multiwavelength observations are key to unveiling the ongoing processes in
IC\,4997 and constraining the origin of the wind variability.
