AAS 196th Meeting, June 2000
Session 4. Young Stars and Their Environments
Display, Monday, June 5, 2000, 9:20am-6:30pm, Empire Hall South

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[4.05] A Dynamical Mass and Distance for a PMS Star: The Binary NTT 045251+3016

A. T. Steffen, R. D. Mathieu (University of Wisconsin - Madison), M. G. Lattanzi (Osservatorio Astronomico di Torino), D. W. Latham (Harvard-Smithsonian Center for Astrophysics), T. Mazeh (Tel Aviv University), L. Prato (UCLA), M. Simon (SUNY, Stony Brook), H. Zinnecker (Astrophysikalisches Institut Potsdam)

We present spectroscopic and astrometric orbital solutions for the pre-main-sequence binary NTT 045251+ 3016. Combination of these data allow the dynamical masses and the distance of the stars to be calculated. Our derived values for the primary and secondary masses are 1.4 ± 0.3 M\odot and 0.8 ± 0.2 M\odot, respectively, at a distance of 139 ± 10 pc. The independently derived distance is consistent with prior distance estimates for the Taurus-Auriga star-forming region.

The primary star is compared with evolutionary tracks of D'Antona and Mazzitelli (1997), Baraffe et al. (1998), and Palla and Stahler (1999) as a preliminary test of PMS evolutionary models. The Baraffe et al. (1998) tracks provide the best fit with our data. The tracks of D'Antona and Mazzitelli (1997) deviate by more than two standard deviations from our result.

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