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Orbital Radial Velocity Curves of Symbiotic Stars

Published online by Cambridge University Press:  12 April 2016

Michael R. Garcia  and
Scott J. Kenyon
Michael R. Garcia
Affiliation:
Harvard/Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA., USA
Scott J. Kenyon
Affiliation:
Harvard/Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA., USA

Abstract

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For the past 6 years we have been measuring the radial velocity of the M-giant component of Symbiotics Stars with high dispersion echelle spectrographs. Because these velocities are based on the absorption line spectrum of the M-star, very reliable orbital radial velocity curves can be constructed. The orbital solutions derived from these velocity curves allow the approximate size of the binary to be determined, and also provide insight into the origin of the photometric variations seen in these stars. For most of the stars, the photometric variations are due to eclipse or reflection effects (two notable exceptions are Z And and RW Hya). Stars which may be near to filling their Roche lobes are TX CVn, Z And, EG And, UV Aur, and CI Cyg. Stars which do not appear to fill their Roche lobes are AG Dra, RW Hya, and AG Peg.

Type
Session 1. The Basic Data
Information
International Astronomical Union Colloquium , Volume 103: The Symbiotic Phenomenon , 1988 , pp. 27 - 32
Copyright
Copyright © Kluwer 1988

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