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On the Separations of Common Proper Motion Binaries Containing White Dwarfs

Published online by Cambridge University Press:  12 April 2016

T.D. Oswalt  and
E.M. Sion
T.D. Oswalt
Affiliation:
Dept. of Physics and Space Sciences FloridaInstitute of Technology Melbourne,Florida,USA32901
E.M. Sion
Affiliation:
Dept. of Astronomy and Astrophysics Villanova University Villanova,Pennsylvania,USA19085

Extract

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Luyten [1,2] and Giclas et al. [3,4] list over 500 known common proper motion binaries (CPMBs) which, on the basis of proper motion and estimated colors, are expected to contain at least one white dwarf (WD) component, usually paired with a late type main sequence (MS) star. Preliminary assessments of the CPMBs suggest that nearly all are physical pairs [5,6]. In this paper we address the issue of whether significant orbital expansion has occurred as a consequence of the post-MS mass loss expected to accompany the formation of the WDs in CPMBs.

Though the CPMB sample remains largely unobserved, a spectroscopic survey of over three dozen CPMBs by Oswalt [5] found that nearly all faint components of Luyten and Giclas color class “a-f” and “+1”, respectively, or bluer were a WD. This tendency was also evident in a smaller sample studied by Greenstein [7]. Conversely, nearly all CPMBs having two components of color class “g-k” and “+3” or redder were MS+MS pairs. With the caveat that such criteria discriminate against CPMBs containing cool (but rare) WDs, they nonetheless provide a crude means of obtaining statistically significant samples for the comparison of orbital separations: 209 highly probable WD+MS pairs and 109 MS+MS pairs.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 454 - 457
Copyright
Copyright © Springer-Verlag 1989

References

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