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We perform general-relativistic hydrodynamical simulations of dynamicalcapture binary neutron star mergers, emphasizing the role played by the neutronstar spin. Dynamical capture mergers may take place in globular clusters, aswell as other dense stellar systems, where most neutron stars have large spins.We find significant variability in the merger outcome as a function of initialneutron star spin. For cases where the spin is aligned with the orbital angularmomentum, the additional centrifugal support in the remnant hypermassiveneutron star can prevent the prompt collapse to a black hole, while forantialigned cases the decreased total angular momentum can facilitate thecollapse to a black hole. We show that even moderate spins can significantlyincrease the amount of ejected material, including the amount unbound withvelocities greater than half the speed of light, leading to brighterelectromagnetic signatures associated with kilonovae and interaction of theejecta with the interstellar medium. Furthermore, we find that the initialneutron star spin can strongly affect the already rich phenomenology in thepostmerger gravitational wave signatures that arise from the oscillation modesof the hypermassive neutron star. In several of our simulations, the resultinghypermassive neutron star develops the one-arm ($m=1$) spiral instability, themost pronounced cases being those with small but non-negligible neutron starspins. For long-lived hypermassive neutron stars, the presence of thisinstability leads to improved prospects for detecting these events throughgravitational waves, and thus may give information about the neutron starequation of state.

Relativistic Simulations of Eccentric Binary Neutron Star Mergers: One-arm Spiral Instability and Effects of Neutron Star Spin