期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 751, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/2041-8205/751/2/L31
关键词
binaries: eclipsing; binaries: spectroscopic; stars: fundamental parameters; stars: individual (Kepler-16); stars: low-mass; techniques: radial velocities
资金
- Center for Exoplanets and Habitable Worlds
- Pennsylvania State University
- Eberly College of Science
- Pennsylvania Space Grant Consortium
- NAI
- PSARC
- NSF [AST-1006676]
We have used high-resolution spectroscopy to observe the Kepler-16 eclipsing binary as a double-lined system and measure precise radial velocities for both stellar components. These velocities yield a dynamical mass ratio of q = 0.2994 +/- 0.0031. When combined with the inclination, i = 90.degrees 3401(-0.0019)(+0.0016), measured from the Kepler photometric data by Doyle et al. (D11), we derive dynamical masses for the Kepler-16 components of M-A = 0.654 +/- 0.017 M-circle dot and M-B = 0.1959 +/- 0.0031 M-circle dot, a precision of 2.5% and 1.5%, respectively. Our results confirm at the similar to 2% level the mass-ratio derived by D11 with their photometric-dynamical model (PDM), q = 0.2937 +/- 0.0006. These are among the most precise spectroscopic dynamical masses ever measured for low-mass stars and provide an important direct test of the results from the PDM technique.
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