Retention Fractions for Globular Cluster Neutron Stars

Abstract

Fokker-Planck models are used to give estimates for the retention fractions for newly-born neutron stars in globular clusters as a function of kick velocity. These can be used to calculate the present day numbers of neutron stars in globular clusters and in addressing questions such as the origin of millisecond pulsars. As an example, the Population I kick velocity distribution of Lyne & Lorimer (1994) is used to estimate the retained fractions of neutron stars originating as single stars and in binary systems. For plausible initial conditions fewer than 4% of single neutron stars are retained. The retention fractions from binary systems can be 2 to 5 times higher. The dominant source of retained neutron stars is found to be through binary systems which remain bound after the first supernova, ie. high-mass X-ray binaries. The retained fraction decreases with an increasing number of progenitors, but the retention fraction decreases more slowly than the number of progenitors increases. On balance, more progenitors give more neutron stars in the cluster.

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