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The Binary Cepheid S Sagittae Revisited

Published online by Cambridge University Press:  12 April 2016

Mark H. Slovak ,
Thomas G. Barnes III ,
Nancy R. Evans ,
Douglas L. Welch  and
Thomas J. Moffett
Mark H. Slovak
Affiliation:
University of Wisconsin, Washburn Observatory
Thomas G. Barnes III
Affiliation:
University of Texas, McDonald Observatory
Nancy R. Evans
Affiliation:
University of Toronto, Department of Astronomy and Computer Science Corporation, Astronomy Programs
Douglas L. Welch
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics
Thomas J. Moffett
Affiliation:
Purdue University, Department of Physics

Abstract

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A new orbit has been derived for the binary Cepheid S Sagittae = HD 188727 = BD+16°4067, using both extant data and new radial velocities derived from radial velocity spectrometer observations at McDonald Observatory and the Dominion Astrophysical Observatory. We deconvoled both the pulsational and orbital components from the observed velocities in order to fit a truncated Fourier series to the pulsation velocities and to derive orbital elements respectively. We confirm the orbital elements given in Herbig and Moore (1952) and speculate that the secular trend evident in the orbital (O-C) diagram may be interpreted as evidence for a third component. (See Evans, Slovak and Welch, this volume, for IUE observations supporting this interpretation.)

Type
4. Abstracts of Poster Papers
Information
International Astronomical Union Colloquium , Volume 111: The Use of Pulsating Stars in Fundamental Problems of Astronomy , 1989 , pp. 284
Copyright
Copyright © Cambridge University Press 1989