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We present the time series photometry of stars located in the extremely young open cluster Berkeley 59. Using the 1.04‐m telescope at Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, we have identified 42 variables in a field of ∼13 × 13 arcmin 2  around the cluster. The probable members of the cluster have been identified using a ( V ,  V − I ) colour–magnitude diagram and a ( J − H ,  H − K ) colour–colour diagram. 31 variables have been found to be pre‐main‐sequence stars associated with the cluster. The ages and masses of the pre‐main‐sequence stars have been derived from the 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 Myr. The masses of these pre‐main‐sequence variable stars have been found to be in the range of ∼0.3 to ∼3.5 M ⊙ , and these could be T Tauri stars. The present statistics reveal that about 90 per cent T Tauri stars have period &lt;15 d. The classical T Tauri stars are found to have a larger amplitude than the weak‐line T Tauri stars. There is an indication that the amplitude decreases with an increase in mass, which could be due to the dispersal of the discs of relatively massive stars.

Photometric search for variable stars in the young open cluster Berkeley 59