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Close encounters between neutron stars and main-sequence stars occur inglobular clusters and may lead to various outcomes. Here we study encountersresulting in tidal disruption of the star. Using $N$-body models, we predictthe typical stellar masses in these disruptions and the dependence of the eventrate on host cluster properties. We find that tidal disruption events occurmost frequently in core-collapsed globular clusters and that roughly $25\%$ ofthe disrupted stars are merger products (i.e., blue straggler stars). Usinghydrodynamic simulations, we model the tidal disruptions themselves (overtimescales of days) to determine the mass bound to the neutron star and theproperties of the accretion disks formed. In general, we find that roughly$80-90\%$ of the initial stellar mass becomes bound to the neutron starfollowing disruption. Additionally, we find that neutron stars receiveimpulsive kicks of up to about $20\,$km/s as a result of the asymmetry ofunbound ejecta; these kicks place these neutron stars on elongated orbitswithin their host cluster, with apocenter distances well outside the clustercore. Finally, we model the evolution of the (hypercritical) accretion disks onlonger timescales (days to years after disruption) to estimate the accretionrate onto the neutron stars and accompanying spin-up. As long as $\gtrsim1\%$of the bound mass accretes onto the neutron star, millisecond spin periods canbe attained. We argue the growing numbers of isolated millisecond pulsarsobserved in globular clusters may have formed, at least in part, through thismechanism. In the case of significant mass growth, some of these neutron starsmay collapse to form low-mass ($\lesssim3\,M_{\odot}$) black holes.

Formation of Low-mass Black Holes and Single Millisecond Pulsars in Globular Clusters