Abstract
Globular clusters contain a relatively large number of low-mass X-ray binaries and low-magnetic-field radiopulsars. This can be understood as a consequence of the high number densities of stars in the cores of some globular clusters. Close encounters between neutron stars and main-sequence or (sub)giant stars lead to the formation of low-mass X-ray binaries, some of which may evolve into binary radiopulsars. If the binary is destroyed, the neutron star — rotating rapidly if it has accreted enough matter from its companion — may become a single radiopulsar. Accurate theoretical predictions of the number of low-mass X-ray binaries in globular clusters are not possible, since the number of neutron stars in globular clusters, and the life time of low-mass X-ray binaries are both uncertain by an order of magnitude.
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