We present the results from an optical spectroscopic analysis of the massive stars HD 37366 and HD 54662. We find that HD 37366 is a double-lined spectroscopic binary with a period of 31.8187 ± 0.0004 days, and HD 54662 is also a double-lined binary with a much longer period of 557.8 ± 0.3 days. The primary of HD 37366 is classified as O9.5 V, and it contributes approximately two-thirds of the optical flux. The less luminous secondary is a broad-lined, early B-type main-sequence star. Tomographic reconstruction of the individual spectra of HD 37366 reveals absorption lines present in each component, enabling us to constrain the nature of the secondary and physical characteristics of both stars. Tomographic reconstruction was not possible for HD 54662; however, we do present mean spectra from our observations that show that the secondary component is approximately half as bright as the primary. The observed spectral energy distributions (SEDs) were fit with model SEDs and galactic reddening curves to determine the angular sizes of the stars. By assuming radii appropriate for their classifications, we determine distance ranges of 1.4-1.9 and 1.2-1.5 kpc for HD 37366 and HD 54662, respectively. © 2007. The American Astronomical Society. All rights reserved.
Publication Source (Journal or Book title)
Boyajian, T., Gies, D., Dunn, J., Farrington, C., Grundstrom, E., Huang, W., McSwain, M., Williams, S., Wingert, D., Fullerton, A., & Bolton, C. (2007). The long-period, massive binaries HD 37366 and HD 54662: Potential targets for long-baseline optical interferometry. Astrophysical Journal, 664 (2 I), 1121-1129. https://doi.org/10.1086/519015