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Observational Evidence for the Origin of X-ray Sources in Globular Clusters

Published online by Cambridge University Press:  01 September 2007

Frank Verbunt ,
Dave Pooley  and
Cees Bassa
Frank Verbunt
Affiliation:
Astronomical Institute, Postbox 80.000, 3508 TA Utrecht, the Netherlands email: verbunt@astro.uu.nl
Dave Pooley
Affiliation:
Dept. of Astronomy, University of Wisconsin-MadisonMadison WI 53706-1582, U.S.A. email: dave@astro.wisc.edu
Cees Bassa
Affiliation:
Physics Department, McGill University, Montreal, QC H3A 2T8Canada email: bassa@physics.mcgill.ca
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Abstract

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Low-mass X-ray binaries, recycled pulsars, cataclysmic variables and magnetically active binaries are observed as X-ray sources in globular clusters. We discuss the classification of these systems, and find that some presumed active binaries are brighter than expected. We discuss a new statistical method to determine from observations how the formation of X-ray sources depends on the number of stellar encounters and/or on the cluster mass. We show that cluster mass is not a proxy for the encounter number, and that optical identifications are essential in proving the presence of primordial binaries among the low-luminosity X-ray sources.

Keywords

X-rays: binariesglobular clusters: generalstellar dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S246: Dynamical Evolution of Dense Stellar Systems , September 2007 , pp. 301 - 310
Copyright
Copyright © International Astronomical Union 2008

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