We propose that the observed difference in the formation rates of bright low-mass X-ray binaries in metal-rich and metal-poor globular clusters can be explained by taking into account the difference in the stellar structure of main sequence donors with masses between \sim 0.85 M _ { \odot } and \sim 1.25 M _ { \odot } at different metallicities .
This difference is caused by the absence of an outer convective zone in metal-poor main sequence stars in this mass range .
In the result , magnetic braking , a powerful mechanism of orbital shrinkage , does not operate and dynamically formed main sequence - neutron star binaries fail to start mass transfer or appear as bright low-mass X-ray binaries .