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The Orbital Period of the Galactic Z Source Sco X-2

Published online by Cambridge University Press:  12 April 2016

K. A. Southwell ,
J. Casares  and
P. A. Charles
K. A. Southwell
Affiliation:
Department of Astrophysics, Nuclear Physics Building, Keble Road, Oxford, 0X1 3RH, UK
J. Casares
Affiliation:
Department of Astrophysics, Nuclear Physics Building, Keble Road, Oxford, 0X1 3RH, UK
P. A. Charles
Affiliation:
Department of Astrophysics, Nuclear Physics Building, Keble Road, Oxford, 0X1 3RH, UK

Abstract

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Sco X-2 is a bright Galactic bulge Z source, whose optical counterpart was discovered in 1990 [?], and observed to exhibit strong Hα emission. We have therefore obtained spectroscopic data in order to determine the orbital period and investigate the nature of the companion star. From an analysis of the Hα emission line velocities, we find a most likely orbital period of 13.94 d. This implies an evolved companion, and is consistent with the currently known orbital periods in other Z sources.

Type
X-Ray Binaries
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 365 - 366
Copyright
Copyright © Kluwer 1996

References

1. Allen, C.W., 1973, Astrophysical Quantities, The Athlone Press, University of London.Google Scholar
2. Penninx, W., Augusteijn, T., 1991, A&A, 246, L81 Google Scholar