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

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

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...196.0405s&link_type=abstract

American Astronomical Society, 196th AAS Meeting, #04.05; Bulletin of the American Astronomical Society, Vol. 32, p.679

Astronomy and Astrophysics

Astronomy

Scientific paper

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 Msun and 0.8 +/- 0.2 Msun, 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.

Affiliated with

Also associated with

No associations

Rating

A Dynamical Mass and Distance for a PMS Star: The Binary NTT 045251+3016 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with A Dynamical Mass and Distance for a PMS Star: The Binary NTT 045251+3016, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A Dynamical Mass and Distance for a PMS Star: The Binary NTT 045251+3016 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1123011