Abstract
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 0 for the white dwarf component, given the calculated mass of 0.24 for the red dwarf component.
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References
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© 1989 Springer-Verlag
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Strand, K.A., Kallarkal, V.V. (1989). The nearby binary, Stein 2051 (G175-34AB). In: Wegner, G. (eds) White Dwarfs. Lecture Notes in Physics, vol 328. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-51031-1_359
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DOI: https://doi.org/10.1007/3-540-51031-1_359
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