We present time-series photometry of stars located in the extremely young open cluster Berkeley 59 . Using the 1.04 m telescope at ARIES , Nainital , we have identified 42 variables in a field of \sim 13 ^ { { } ^ { \prime } } \times 13 ^ { { } ^ { \prime } } around the cluster . The probable members of the cluster are identified using ( V,V - I ) colour-magnitude diagram and ( J - H,H - K ) colour-colour diagram . Thirty one variables are found to be pre-main sequence stars associated with the cluster . The ages and masses of pre-main sequence stars are derived from colour-magnitude diagram by fitting theoretical models to the observed data points . The ages of the majority of the probable pre-main sequence variable candidates range from 1 to 5 Myrs . The masses of these pre-main sequence variable stars are found to be in the range of \sim 0.3 to \sim 3.5 M _ { \odot } and these could be T Tauri stars . The present statistics reveal that about 90 % T Tauri stars have periods < 15 days . The classical T Tauri stars are found to have larger amplitude in comparison to the weak line T Tauri stars . There is an indication that the amplitude decreases with increase of the mass , which could be due to the dispersal of disk of relatively massive stars .