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Using general-relativistic hydrodynamical simulations, we show that mergingbinary neutron stars can form hypermassive neutrons stars that undergo theone-arm spiral instability. We study the particular case of a dynamical capturemerger where the stars have a small spin, as may arise in globular clusters,and focus on an equal-mass scenario where the spins are aligned with theorbital angular momentum. We find that this instability develops whenpost-merger fluid vortices lead to the generation of a toroidal remnant - aconfiguration whose maximum density occurs in a ring around the center-of-mass- with high vorticity along its rotation axis. The instability quicklysaturates on a timescale of $\sim 10$ ms, with the $m=1$ azimuthal densitymultipole mode dominating over higher modes. The instability also leaves acharacteristic imprint on the post-merger gravitational wave signal that couldbe detectable if the instability persists in long-lived remnants.

One-arm Spiral Instability in Hypermassive Neutron Stars Formed by Dynamical-Capture Binary Neutron Star Mergers