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Secondaries of eclipsing binaries. IV - The triple system Lambda Tauri
Fekel, F. C., Jr.; Tomkin, J.
AA(NASA, Goddard Space Flight Center, Laboratory for Astronomy and Solar Physics, Greenbelt, MD), AB(Texas, University, Austin, TX)
Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 289-301. NASA-supported research (ApJ Homepage)
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NASA/STI Keywords:
Eclipsing Binary Stars, Orbit Calculation, Orbital Elements, Radial Velocity, Stellar Motions, Dwarf Stars, K Stars, Stellar Mass, Stellar Spectra, Three Body Problem
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High signal-to-noise ratio Reticon observations of Lambda Tauri have been obtained along with high-quality orbital elements for both the primary and secondary of the eclipsing system. The velocity curve of the secondary is determined for the first time. The findings include: K(1) = 56.9 + or - 0.6 km/s, K(2 = 215.6 + or - 0.7 km/s, m(1) = 7.18 + or - 0.09 solar masses, and m(2) = 1.89 + or - 0.04 solar masses. The 33-day periodicity in the residuals is confirmed and is present in the secondary velocities as well as those of the primary, and can unambiguously be ascribed to orbital motion about a third body. The K and f(m) for the 33-day orbit are 10.1 + or - 0.7 km/s and 0.0034 + or - 0.0008 solar masses. The photometry shows that the orbits are coplanar to within seven degrees. The mass of the third body is 0.7 + or - 0.2 solar masses; it is most probably a K dwarf.

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