MASSES AND DISTANCE OF THE YOUNG BINARY NTTS 045251+3016

Journal Article · Sat Aug 10 00:00:00 EDT 2013 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/773/1/28· OSTI ID:22140283

Simon, M. ^[1]; Schaefer, G. H. ^[2]; Prato, L.; Ruiz-Rodriguez, Dary; Karnath, N.; Franz, O. G.

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1. Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800 (United States)
2. The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, CA 91023 (United States)

As part of our continuing campaign to measure the masses of pre-main-sequence (PMS) stars dynamically and thus to assess the reliability of the discrepant theoretical calculations of contraction to the main sequence, we present new results for NTTS 045251+3016, a visual and double-lined spectroscopic binary in the Taurus star-forming region (SFR). We obtained new high angular resolution astrometry and high spectral resolution spectroscopy at Keck Observatory. The new data lead to a significant revision of previously published orbital parameters. In particular, we find that the masses of the primary and secondary are 0.86 {+-} 0.11 and 0.55 {+-} 0.05 M{sub Sun }, respectively, smaller than previously reported, and that the system lies 158.7 {+-} 3.9 pc from the sun, further than previously reported.

• OSTI ID: 22140283
• Journal Information: Astrophysical Journal, Vol. 773, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
BINARY STARS
MASS
RELIABILITY
RESOLUTION
SPECTROSCOPY
SUN