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Determination of stellar age is a crucial task in astrophysics research.Different methods are nowadays used either model dependent or based oncalibrated empirical relations. The most reliable results are generallyobtained when different methods are used in complementary way. We propose a newmethod for the age determination of young stellar associations and openclusters (ages < 125 Myr), which can allow to further constrain the age whenused together with other methods. We explore the amplitude of the photometricvariability in bins of color and rotation period of five young associations andclusters spanning an interval of ages from 1-3 Myr to 625 Myr (Taurus, rhoOphiuchi, Upper Scorpius, Pleiades, and Praesepe), which all have high-qualitytime-series photometry from Kepler K2 campaigns. In the low-mass regime, wefind that stars with similar color and rotation period but different agesexhibit different amplitudes of their photometric variability, with youngerstars showing a larger photometric variability than older stars. The decline ofphotometric variability amplitude versus age in stars with similar color androtation period can be in principle calibrated and be adopted as an additionalempirical relation to constrain the age of young associations and openclusters, provided that time-series photometry is available for their low-massmembers.

Constraining the age of young stellar clusters via the amplitude of photometric variability