Other
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..823g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 2, p. 823-830
Other
14
Binary Stars, Emission Spectra, Line Spectra, Mass Ratios, O Stars, Orbital Elements, Radial Velocity, Stellar Magnitude, Stellar Mass, Absorption Spectra, Astronomical Spectroscopy, Helium, Hydrogen, Tomography
Scientific paper
We present radial velocities and line profiles of the O-type star HD 53975, which we find to be a spectroscopic binary with a period of 6.0173 days. Although there are no obvious signatures of the secondary in the line profiles, we have used the merit function of Shafter et al. (1980) to show that a secondary component is present in lines found in B-type spectra. We have compared the observed merit functions with merit functions for model profiles constructed assuming a main-sequence secondary, and this comparison consistently indicates a companion with a mass ratio of q = M2/M1 = 0.23 +/- 0.04 and a magnitude difference Delta m = 3.3 +/- 0.4. We present a tomographic reconstruction of the spectrum of the secondary for these parameters. We suggest that other large mass ratio binaries may be found among the O stars when observed with high-resolution and high signal-to-noise ratio spectroscopy.
Bagnuolo William G. Jr.
Bolton Charles T.
Fullerton Alex W.
Gies Douglas R.
Hahula Michael E.
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