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We present an astrometric/spectroscopic orbital solution for thepre-main-sequence binary NTT 045251+3016. Our measurements for the primary andsecondary masses are 1.45 +/- 0.19 M_sun and 0.81 +/- 0.09 M_sun, respectively,and 145 +/- 8 pc for the distance of the system, consistent with priorestimates for the Taurus-Auriga star-forming region. The evolutionary tracks ofD'Antona & Mazzitelli (1997), Baraffe et al. (1998), and Palla & Stahler (1999)are tested against these dynamical mass measurements. Due to the intrinsiccolor/T_eff variation within the K5 spectral class, each pre-main-sequencemodel provides a mass range for the primary. The theoretical mass range derivedfrom the Baraffe et al. (1998) tracks that use a mixing length parameteralpha=1.0 is closest to our measured primary mass, deviating between 1.3 and1.6 sigma. The set of Baraffe et al. (1998) tracks that use alpha=1.9 deviatebetween 1.6 and 2.1 sigma from our measured primary mass. The mass range givenby the Palla & Stahler (1999) tracks for the primary star deviate between 1.6and 2.9 sigma. The D'Antona & Mazzitelli (1997) tracks give a mass range thatdeviates by at least 3.0 sigma from our derived primary mass, stronglysuggesting that these tracks are inconsistent with our observation.Observations of the secondary are less constraining than those of the primary,but the deviations between the dynamical mass of the secondary and the massinferred for the secondary from the various pre-main-sequence tracks mirror thedeviations of the primary star. All of the pre-main-sequence tracks areconsistent with coevality of the components of NTT 045251+3016.Comment: 27 pages, 6 figures, 5 tables -- accepted by A

A Dynamical Mass Constraint for Pre–Main-Sequence Evolutionary Tracks: The Binary NTT 045251+3016