Overview of Multiple Star Systems

Mathieu, Robert D.

doi:10.1007/978-3-662-47290-3_9

Robert D. Mathieu⁸

Part of the book series: Saas-Fee Advanced Course ((SAASFEE,volume 42))

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Abstract

Multiple stars represent approximately 50 % of the stellar population, and as a result, have implications for the dynamics of young star clusters and associations. This chapter reviews several aspects of multiple star systems, namely the field solar-type multiple population, the field OB star multiple population, and finally the open cluster solar-type multiple population. We discuss each in terms of observed distributions and how these vary depending on their environment. Finally, we close with some thoughts concerning the significance of multiple star systems to the dynamics of young star clusters and associations, specifically how these can be used to further constrain star formation processes and whether these systems can be used as a tracer of identifying the origin of the field population.

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Notes

1.
There are many ways to do the accounting of multiplicity. Here we use a simple approach: a ‘star system’ may be single (no detected companions), or binary, or triple, or quadruple, or perhaps a higher-order system. The frequency of multiple systems is defined as the number of multiple systems divided by all such ‘star systems’ examined.
2.
Almost all field star multiple systems are hierarchical, as required for dynamical stability. Thus there is no ambiguity, for example, in identifying two distinct binary pairings within a triple system, or three within a quadruple system.
3.
This result harkens back to Blaauw’s manuscript in which the vast majority of OB stars in associations were claimed to be spectroscopic binaries. There is cause to have caution regarding such results. If one happens to be optimistic about one’s external precision, particularly if it is determined from internal precisions, one’s spectroscopic binary detection rate will be inflated. Nonetheless, this result of high binary frequency among OB stars has survived the years.
4.
These data and results for M35 are those of the WIYN Open Cluster Study and the radial velocity measurements are published in Geller et al. (2010). The papers with the binary orbits and population distributions are from (Leiner et al. 2015).

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Department of Astronomy, University of Wisconsin, Madison, WI, USA
Robert D. Mathieu

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Robert D. Mathieu
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Correspondence to Robert D. Mathieu .

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Institute for Astronomy,ETH, Zürich, Switzerland
Michael R. Meyer
Department of Astronomy of Geneva Univer, Geneva Observatory, Sauverny, Switzerland
Laurent Eyer
Department of Physics & Astronomy, University of Rochester, Rochester, USA
Cameron P.M. Bell

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Mathieu, R.D. (2015). Overview of Multiple Star Systems. In: Meyer, M., Eyer, L., Bell, C. (eds) Dynamics of Young Star Clusters and Associations. Saas-Fee Advanced Course, vol 42. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-47290-3_9

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DOI: https://doi.org/10.1007/978-3-662-47290-3_9
Published: 12 September 2015
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-662-47289-7
Online ISBN: 978-3-662-47290-3
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