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Neutron Stars in Globular Clusters

Published online by Cambridge University Press:  01 September 2007

N. Ivanova ,
C. O. Heinke  and
F. Rasio
N. Ivanova
Affiliation:
CITA, University of Toronto, 60 St George St, Toronto, ON M5R 2N6, Canada email: nata@cita.utoronto.ca
C. O. Heinke
Affiliation:
Department of Astronomy, University of Virginia, 530 McCormick Road Charlottesville, VA 22904-4325, USA email: cheinke@virginia.edu Physics and Astronomy Department, Northwestern University, 2145 Sheridan Rd, Evanston, IL 60208USA email: rasio@northwestern.edu
F. Rasio
Affiliation:
Physics and Astronomy Department, Northwestern University, 2145 Sheridan Rd, Evanston, IL 60208USA email: rasio@northwestern.edu
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Abstract

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Dynamical interactions that occur between objects in dense stellar systems are particularly important for the question of formation of X-ray binaries. We present results of numerical simulations of 70 globular clusters with different dynamical properties and a total stellar mass of 2×107M⊙. We find that in order to retain enough neutron stars to match observations we must assume that NSs can be formed via electron-capture supernovae. Our simulations explain the observed dependence of the number of LMXBs on “collision number” as well as the large scatter observed between different globular clusters. For millisecond pulsars, we obtain good agreement between our models and the numbers and characteristics of observed pulsars in the clusters Terzan 5 and 47 Tuc.

Keywords

binaries: closeglobular clusters: generalX-rays: binaries

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