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Published December 15, 2015 | Published
Journal Article Open

Binary neutron stars with arbitrary spins in numerical relativity

Abstract

We present a code to construct initial data for binary neutron star systems in which the stars are rotating. Our code, based on a formalism developed by Tichy, allows for arbitrary rotation axes of the neutron stars and is able to achieve rotation rates near rotational breakup. We compute the neutron star angular momentum through quasilocal angular momentum integrals. When constructing irrotational binary neutron stars, we find a very small residual dimensionless spin of ∼2×10^(−4). Evolutions of rotating neutron star binaries show that the magnitude of the stars' angular momentum is conserved, and that the spin and orbit precession of the stars is well described by post-Newtonian approximation. We demonstrate that orbital eccentricity of the binary neutron stars can be controlled to ∼0.1%. The neutron stars show quasinormal mode oscillations at an amplitude which increases with the rotation rate of the stars.

Additional Information

© 2015 American Physical Society. (Received 28 August 2015; published 9 December 2015) We thank Rob Owen and Geoffrey Lovelace for discussions on quasilocal spins. Calculations were performed with the Spectral Einstein Code (spec) [83]. We gratefully acknowledge support for this research at CITA from NSERC of Canada, the Canada Research Chairs Program, the Canadian Institute for Advanced Research, and the Vincent and Beatrice Tremaine Postdoctoral Fellowship (F. F.); at LBNL from NASA through Einstein Postdoctoral Fellowship Grant No. PF4-150122 (F. F.) awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060; at Caltech from the Sherman Fairchild Foundation and NSF Grants No. PHY-1440083, No. PHY-1404569, No. PHY-1068881, No. CAREER PHY-1151197, TCAN No. AST-1333520, and NASA ATP Grant No. NNX11AC37G; at Cornell from the Sherman Fairchild Foundation and NSF Grants No. PHY-1306125 and No. AST-1333129; and at WSU from NSF Grant No. PHY-1402916. Calculations were performed at the GPC supercomputer at the SciNet HPC Consortium [84]; SciNet is funded by the Canada Foundation for Innovation (CFI) under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund (ORF)–Research Excellence; and the University of Toronto. Further calculations were performed on the Briarée cluster at Sherbrooke University, managed by Calcul Québec and Compute Canada and with operation funded by the Canada Foundation for Innovation (CFI), Ministére de l'Économie, de l'Innovation et des Exportations du Quebec (MEIE), RMGA and the Fonds de recherche du Québec—Nature et Technologies (FRQ-NT); on the Zwicky cluster at Caltech, which is supported by the Sherman Fairchild Foundation and by NSF Award No. PHY-0960291; on the NSF XSEDE network under Grant No. TG-PHY990007N; on the NSF/NCSA Blue Waters at the University of Illinois with allocation jr6 under NSF PRAC Award No. ACI-1440083.

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Published - PhysRevD.92.124012.pdf

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Created:
August 20, 2023
Modified:
October 25, 2023