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|Abstract:||Using general-relativistic hydrodynamical simulations, we show that merging binary neutron stars can form hypermassive neutrons stars that undergo the one-arm spiral instability. We study the particular case of a dynamical capture merger 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 the orbital angular momentum. We find that this instability develops when postmerger fluid vortices lead to the generation of a toroidal remnant-a configuration whose maximum density occurs in a ring around the center-of-mass-with high vorticity along its rotation axis. The instability quickly saturates on a time scale of similar to 10 ms, with the m = 1 azimuthal density multipole mode dominating over higher modes. The instability also leaves a characteristic imprint on the postmerger gravitational wave signal that could be detectable if the instability persists in long-lived remnants.|
|Electronic Publication Date:||30-Dec-2015|
|Citation:||Paschalidis, Vasileios, East, William E, Pretorius, Frans, Shapiro, Stuart L. (2015). One-arm spiral instability in hypermassive neutron stars formed by dynamical-capture binary neutron star mergers. PHYSICAL REVIEW D, 92 (10.1103/PhysRevD.92.121502|
|Type of Material:||Journal Article|
|Journal/Proceeding Title:||PHYSICAL REVIEW D|
|Version:||Final published version. Article is made available in OAR by the publisher's permission or policy.|
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