The Spectroscopic Orbit of the Evolved Binary HD197770

Karl D. Gordon; Geoffrey C. Clayton; Tracy L. Smith; Jason P. Aufdenberg; John S. Drilling; Margaret M. Hanson; Christopher M. Anderson; Christopher L. Mulliss

doi:10.1086/300385

The Spectroscopic Orbit of the Evolved Binary HD 197770

Karl D. Gordon¹, Geoffrey C. Clayton¹, Tracy L. Smith², Jason P. Aufdenberg³, John S. Drilling¹, Margaret M. Hanson^4,5, Christopher M. Anderson⁶, and Christopher L. Mulliss²

© 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A.
The Astronomical Journal, Volume 115, Number 6 Citation Karl D. Gordon et al 1998 AJ 115 2561 DOI 10.1086/300385

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Author affiliations

¹ Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803

² Department of Physics and Astronomy, Ritter Observatory 405, University of Toledo, Toledo, OH 43606

³ Department of Physics and Astronomy, Arizona State University, Box 871504, Tempe, AZ 85287

⁴ Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721

⁵ Hubble Postdoctoral Fellow

⁶ Department of Physics and Astronomy and Space Astronomy Laboratory, University of Wisconsin at Madison, 475 North Charter Street, Madison, WI 53706

Dates

Received 1998 February 2

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Abstract

We have used spectra taken between 1992 and 1997 to derive the spectroscopic orbit of the eclipsing double-lined spectroscopic binary HD 197770. This binary has a period of 99.69 ± 0.02 days and K amplitudes of 31.2 ± 0.8 and 47.1 ± 0.4 km s^-1 for components A and B, respectively. The m sin³ i values for A and B are 2.9 and 1.9, respectively, and are close to the actual masses because of the eclipsing nature of this binary. Both components of HD 197770 have spectral types near B2 III. This means that both components are undermassive by about a factor of 5 and, thus, are evolved stars. Additional evidence of the evolved nature of HD 197770 is found in 25, 60, and 100 μm IRAS images of HD 197770. These images show two apparent shells centered on HD 197770, a bright 60 μm shell with a 28' diameter and a larger (0 fdg 8 diameter) bubble-like feature. At least one of the components of HD 197770 is likely to be a post–asymptotic giant branch star.

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