Photometric observations of HD 217522 in 1981 revealed only one pulsation frequency \nu _ { 1 } = 1.21529 mHz .
Subsequent observations in 1989 showed the presence of an additional frequency \nu _ { 2 } = 2.0174 mHz .
New observations in 2008 confirm the presence of the mode with \nu _ { 2 } = 2.0174 mHz .
Examination of the 1989 data shows amplitude modulation over a time scale of the order of a day , much shorter than what has been observed in other roAp stars .
High spectral and time resolution data obtained using the VLT in 2008 confirm the presence of \nu _ { 2 } and short term modulations in the radial velocity amplitudes of rare earth elements .
This suggests growth and decay times shorter than a day , more typical of solar-like oscillations .
The driving mechanism of roAp stars and the Sun are different , and the growth and decay seen in the Sun are due to stochastic nature of the driving mechanism .
The driving mechanism in roAp stars usually leads to mode stability on a longer time-scale than in the Sun .
We interpret the reported change in \nu _ { 1 } between the 1982 and 1989 data as part of the general frequency variability observed in this star on many time scales .