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The Spectroscopic orbit of ϕ Cygni, A System with two Late-Type Giants

Published online by Cambridge University Press:  22 February 2018

Francis C. Fekel
Francis C. Fekel*
Affiliation:
Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, USA. email: fekel@evans.tsuniv.edu

Abstract

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Improved orbital elements for ϕ Cygni have been determined from 47 new high-dispersion spectroscopic observations. The period and eccentricity are 434.14 days and 0.559, respectively. Minimum masses plus the inclination of the visual orbit result in masses of 2.16 and 2.06 M⊙ for the two giants. The small magnitude difference of 0.25 mag and a mass ratio of 1.044 indicate that both giants are most likely in the helium-burning phase of their evolution.

Resumen

Resumen

Se han determinado elementos orbitales mejorados para ϕ Cygni, mediante 47 nuevas observaciones espec-troscópicas. El período es 434.14 días y la excentricidad 0.559. Con las masas mínimas y la inclinación de la órbita visual obtenemos masas de 2.16 y 2.06 M⊙ para las dos gigantes. La pequeña diferencia de magnitudes (0.25 mag) y el cociente de masas (1.044) indican que ambas gigantes se encuentran en la fase evolutiva del quemado del helio.

Keywords

BinariesClose — BinariesSpectroscopic
Type
Observational properties and Statistics of Binary Stars in the Field
Information
International Astronomical Union Colloquium , Volume 191: The Environment and Evolution of Double and Multiple Stars , August 2004 , pp. 63 - 64
Copyright
Copyright © Instituto de Astronomia – Mexico 2004

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