THE PRE-MAIN-SEQUENCE SPECTROSCOPIC BINARY NTTS-162814-2427 - MODELS VERSUS OBSERVATIONS

Models of stars with masses between 0.5 and 1.5 M. evolving in the pre -main-sequence (PMS) have been computed using a multiple shooting poin t hydrodynamic code. The theoretical results are compared with the mos t recent observational data available for the double-lined PMS spectro scopic binary NTTS 162814-2427. A comparison with theoretical models c omputed with different input physics concerning the opacities, the equ ation of state (EOS) and the convection treatment of superadiabatic re gions is also done. Our reference model agrees well with the dynamical mass ratio and the assumption of coeval formation of the binary compo nents. Accordingly, assuming a K4 primary and a K5 secondary we estima te the mass of the primary and secondary to be 1.10 and 1.00 M., respe ctively, with an age of 3.7 million years.