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The Nearby Binary, Stein 2051 (G175–34AB)

Published online by Cambridge University Press:  12 April 2016

K. Aa. Strand  and
V. V. Kallarkal
K. Aa. Strand
Affiliation:
3200 Rowland Place, NW WashingtonD.C. 20008
V. V. Kallarkal
Affiliation:
U.S. Naval Observatory Washington, D.C. 20392

Abstract

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Photographic observations of the large proper motion binary, Stein 2051, extended over the period 1966–87, do not support that it is a triple system as previously reported (Strand, 1977). The orbital motion is nearly linear over this interval? however, when results of plates from the Vatican Astrographic Zone from 1908–11 are included, a mass ratio is obtained, leading to a mass of 0.50©for the white dwarf component, given the calculated mass of 0.24© for the red dwarf component.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 413 - 415
Copyright
Copyright © Springer-Verlag 1989

References

Eggen, O.J., Greenstein, J.L.: 1967, Astrophys.J. 150, 927 Google Scholar
Giclas, H.L., Bunham, R. Jr., Thomas, N.G.: 1965, Lowell Obs. Bull. No. 129 Google Scholar
Hardie, R.H., Heiser, A.M.: 1966, Publ. Astron. Soc. Pacific 78, 171 Google Scholar
Harrington, R.S., Christy, J.W., Strand, K.Aa.: 1981, Astron.J. 86, 909 Google Scholar
Liebert, J.: 1976, Astrophys.J. 210, 215 CrossRefGoogle Scholar
Strand, K.Aa.: 1977, Astron.J. 82, 745 CrossRefGoogle Scholar