AAS 203rd Meeting, January 2004
Session 12 Eclipsing Binary Stars
Poster, Monday, January 5, 2004, 9:20am-6:30pm, Grand Hall

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[12.11] The Components of the HD 206267 A Triple Star System

J. A. Harvin (University of Delaware), D. R. Gies (Georgia State University), L. R. Penny (College of Charleston)

We present double-lined spectroscopic orbital elements for the central binary in the massive multiple star, HD~206267 based on fits of cross-correlation functions of the 36 IUE high dispersion UV spectra available. These elements give masses for the primary and secondary components of m1 \sin3 i = 28.0 M\odot ± 1.8 and m2 \sin3 i = 15.3 M\odot ±1.5. We also present tomographic reconstructions of all three spectroscopic components that confirm the O6.5~V((f)) classification of the composite spectrum applies to the primary, indicate a B0~V type for the secondary, and an O8~V type for the tertiary. The relative line strengths between the reconstructed spectra suggest magnitude differences of \Delta m = -2.5 \log (Fs/Fp) = 1.4 ±0.2 in the UV and \Delta m = 1.2 ±0.3 in the optical for the secondary and \Delta m = -2.5 \log (Ft/Fp) = 1.2 ±0.2 in the UV and \Delta m = 1.0 ± 0.3 in the optical for the tertiary. The widths of the UV cross-correlation functions are used to estimate the projected rotational velocities, Vp\sin i = 192 ±22 {\rm ~km~s}-1, Vs\sin i = 109 ±23 {\rm ~km~s}-1, and Vt\sin i = 117 ±23 {\rm ~km~s}-1 for the components. The Hipparcos photometry of HD~206267 is inconclusive regarding the nature of its light variations, and so, only upper limits can be found. If the system eclipses, the inclination could be as high as i = 65\circ, otherwise, i = 55\circ or less.

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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.