Orbital Solutions for Two Young, Low-Mass Spectroscopic Binaries in Ophiuchus

Details Orbital Solutions for Two Young, Low-Mass Spectroscopic Binaries in Ophiuchus Orbital Solutions for Two Young, Low-Mass Spectroscopic Binaries in Ophiuchus

2010-10-31

arxiv.org/abs/1011.0193v2

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Accepted for publication in the AJ; 8 figures. Corrected typos in Table 5

Scientific paper

We report the orbital parameters for ROXR1 14 and RX J1622.7-2325Nw, two young, low-mass, and double-lined spectroscopic binaries recently discovered in the Ophiuchus star forming region. Accurate orbital solutions were determined from over a dozen high-resolution spectra taken with the Keck II and Gemini South telescopes. These objects are T Tauri stars with mass ratios close to unity and periods of ~5 and ~3 days, respectively. In particular, RX J1622.7-2325Nw shows a non-circularized orbit with an eccentricity of 0.30, higher than any other short-period pre-main sequence spectroscopic binary known to date. We speculate that orbit of RX J1622.7-2325Nw has not yet circularized because of the perturbing action of a ~1" companion, itself a close visual pair. A comparison of known young spectroscopic binaries and main sequence (MS) spectroscopic binaries in the eccentricity-period plane shows an indistinguishable distribution of the two populations, implying that orbital circularization occurs in the first 1 Myr of a star's lifetime. With the results presented in this paper we are increasing by ~4% the small sample of PMS spectroscopic binary stars with known orbital elements.

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