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There are a variety of different techniques available to estimate the ages ofpre-main-sequence stars. Components of physical pairs, thanks to their strictcoevality and the mass difference, such as the binary system analysed in thispaper, are best suited to test the effectiveness of these different techniques.We consider the system WW Psa + TX Psa whose membership of the 25-Myr betaPictoris association has been well established by earlier works. We investigatewhich age dating technique provides the best agreement between the age of thesystem and that of the association. We have photometrically monitored WW Psaand TX Psa and measured their rotation periods as P = 2.37d and P = 1.086d,respectively. We have retrieved from the literature their Li equivalent widthsand measured their effective temperatures and luminosities. We investigatewhether the ages of these stars derived using three independent techniques areconsistent with the age of the beta Pictoris association. We find that therotation periods and the Li contents of both stars are consistent with thedistribution of other bona fide members of the cluster. On the contrary, theisochronal fitting provides similar ages for both stars, but a factor of aboutfour younger than the quoted age of the association, or about 30% younger whenthe effects of magnetic fields are included. We explore the origin of thediscrepant age inferred from isochronal fitting, including the possibilitiesthat either the two components may be unresolved binaries or that the basicstellar parameters of both components are altered by enhanced magneticactivity. The latter is found to be the more reasonable cause, suggesting thatage estimates based on the Li content is more reliable than isochronal fittingfor pre-main-sequence stars with pronounced magnetic activity.

On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association