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Through the modelling of near-infrared photometry of star plus disk systemswith the codes BEDISK/BERAY, we successfully describe the WISE photometriccharacteristics of Be stars in five young open clusters, NGC 663, NGC 869, NGC884, NGC 3766 and NGC 4755, broadly studied in the literature. WISE photometryallows previously known Be stars to be detected and to find new Be candidateswhich could be confirmed spectroscopically. The location of Be stars in theWISE colour-magnitude diagram, separates them in two groups; active (Be starshosting a developed circumstellar disk) and quiescent objects (Be stars in adiskless phase), and this way, we can explore how often stars are observed inthese different stages. The variability observed in most active variable Bestars is compatible with a disk dissipation phase. We find that 50 percent ofBe stars in the studied open clusters are in an active phase. We can interpretthis as Be stars having a developed circumstellar disk half of the time. Thelocation of Be stars with a developed disk in the CMD require mass loss ratesin agreement with values recently reported in the literature. For theseobjects, we expect to have a tight relation between the equivalent width of theH{\alpha} line and the mass of the disk, if the inclination is known. Also,near-infrared photometry of Be stars in stellar clusters has the potential ofbeing useful to test whether there is a preferential viewing angle.

Quiescent and active phases in Be stars: A WISE snapshot of young galactic open clusters