## 6. ConclusionsWe have compared the most recent observational data available for the double-lined PMS binary NTTS 162814-2427 with theoretical models using different input physics for the opacities, the equation of state and the treatment of superadiabatic convection. All models, except the one computed without Coulomb corrections in the EOS, are in good agreement with the dynamical mass ratio and the assumption of coeval formation of the binary components. Thus, although the observational data are not able to provide tight constraints to the input physics used in the stellar evolution models, namely on the choice of the opacity sets and the treatment of superadiabatic convection used, they are nevertheless able to corroborate the importance of including the effects of Coulomb interactions between charged particles while computing the EOS. Our results also show that the main contribution to the uncertainties in the mass and age determinations comes from the observational uncertainties, which are considerably higher than the theoretical ones. Therefore, more accurate determinations of effective temperatures and luminosities would be very useful to provide better mass and age estimates, and tighter constraints to the theoretical models. Assuming a K4 primary and a K5 secondary, models differing only in the values of the opacity used lead to similar mass-age calibrations. In particular, our reference model yields: , and an age of the order of 3.7 million years for the binary system. The values resulting from the CM convection treatment with are only slightly higher: , , and an age of the order of 4.0 million years. © European Southern Observatory (ESO) 1997 Online publication: July 3, 1998 |