Abstract
Observations of galactic and extra-galactic globular clusters have shown that on average metal-rich clusters are ~3 times as likely to contain a bright X-ray source than their metal-poor counterparts. We propose that this can be explained by taking into account the difference in the stellar structure of main sequence donors with masses between ~0.85 Msun and ~1.25 Msun at different metallicities. Metal-poor main sequence stars in this mass range do not have an outer convective zone while metal-rich stars do. The absence of this zone turns off magnetic braking, a powerful mechanism of orbital shrinkage, leading to the failure of dynamically formed main sequence - neutron star binaries to start mass transfer or appear as bright low-mass X-ray binaries.
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