  Variability is a commonly observed property of classical Be stars (CBe)
stars. In extreme cases, complete disappearance of the H{\alpha} emission line
occurs, indicating a disc-less state in CBe stars. The disc-loss and
reappearing phases can be identified by studying the H{\alpha} line profiles of
CBe stars on a regular basis. In this paper, we present the study of a set of
selected 9 bright CBe stars, in the wavelength range of 6200 - 6700 {\AA}, to
better understand their disc transient nature through continuous monitoring of
their H{\alpha} line profile variations for 5 consecutive years (2015 -- 2019).
Based on our observations, we suggest that 4 of the program stars (HD 4180, HD
142926, HD 164447 and HD 171780) are possibly undergoing disc-loss episodes,
whereas one other star (HD 23302) might be passing through disc formation
phase. The remaining 4 stars (HD 237056, HD 33357, HD 38708 and HD 60855) have
shown signs of hosting a stable disc in recent epochs. Through visual
inspection of the overall variation observed in the H{\alpha} EW for these
stars, we classified them into groups of growing, stable and dissipating discs,
respectively. Moreover, our comparative analysis using the BeSS database points
out that the star HD 60855 has passed through a disc-less episode in 2008, with
its disc formation happening probably over a timescale of only 2 months,
between January and March 2008.

Solar and Stellar Astrophysics