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Spectroscopic Binaries in the Halo

Published online by Cambridge University Press:  12 April 2016

David W. Latham ,
Tsevi Mazeh ,
Robert P. Stefanik ,
Robert J. Davis ,
Bruce W. Carney ,
Guillermo Torres  and
John B. Laird
David W. Latham
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Tsevi Mazeh
Affiliation:
School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Science, Tel Aviv University, Tel Aviv 69978, Israeland Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Robert P. Stefanik
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Robert J. Davis
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Bruce W. Carney
Affiliation:
Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA
Guillermo Torres
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA and Cördoba Observatory, National University of Cördoba, Laprida 854, 5000 Cördoba, Argentina
John B. Laird
Affiliation:
Department of Physics and Astronomy, Bowling Green State University, Bowling Green, Ohio 43403

Abstract

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For almost 1500 stars in the Carney-Latham survey of proper-motion stars we have accumulated about 20,000 precise radial velocities. Already we have orbital solutions for more than 150 spectroscopic binaries in this sample, and about 100 additional binary candidates with variable velocity. We find that among the metal-poor halo field stars in this sample the frequency of short-period spectroscopic binaries is indistinguishable from that of the disk. The distribution of eccentricity versus period shows evidence for tidal circularization on the main sequence. For the binaries more metal poor than [m/H] = −1.6 there is a clean transition from circular to elliptical orbits at a period of about 19 days. For longer periods the distribution of eccentricity is the same as for stars in the disk of the Galaxy.

Type
Spectroscopic Studies
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 158 - 160
Copyright
Copyright © Astronomical Society of the Pacific 1992

References

Ardeberg, A. & Lindgren, H. 1991, A&A, 244, 310 Google Scholar
Carney, B.W. & Latham, D.W. 1987, AJ, 93, 116 CrossRefGoogle Scholar
Duquennoy, A. & Mayor, M. 1991, A&A, 248, 485 Google Scholar
Latham, D.W., Mazeh, T., Carney, B.W., McCrosky, R.E., Stefanik, R.P., & Davis, R.J. 1988, AJ, 96, 567 CrossRefGoogle Scholar
Latham, D.W., Mazeh, T., Stefanik, R.P., Davis, R.J., Carney, B.W., Krymolowski, Y.,Laird, J.B., Torres, G., & Morse, J.A. 1992, AJ, 104, 774 CrossRefGoogle Scholar
Mathieu, R.D., Duquennoy, A., Latham, D.W., Mayor, M., Mazeh, T., Mermilliod, J.-C. 1992, In Workshop on Binaries as Tracers of Stellar Formation and Evolution, eds. Duquennoy, A. and Mayor, M. (Cambridge, Cambridge University Press), in pressGoogle Scholar
Mathieu, R.D. & Mazeh, T. 1988, ApJ, 326, 256 Google Scholar
Morrison, H.L., Flynn, C., & Freeman, K.C., 1990, AJ, 100, 1191 CrossRefGoogle Scholar
Stefanik, R.P. & Latham, D.W. 1992, this ColloquiumGoogle Scholar
Torres, G. 1991, PhD thesisGoogle Scholar
Zahn, J.-P. 1977, A&A, 57, 383 Google Scholar