Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the spin orientation

2020/03/31 by Swami Vivekanandji Chaurasia, Tim Dietrich, Maximiliano Ujevic +5
Physics and Astronomy · #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics #Classical mechanics #Computational physics #Condensed matter physics #Gamma-ray bursts and supernovae #Gravitational wave #Moment of inertia #Neutron star #Orbital motion #Orbital plane #Physics #Precession #Pulsars and Gravitational Waves Research #Quantum mechanics #Spin (aerodynamics) #Spins #astro-ph.HE #gr-qc

paper · pdf · doi:10.1103/physrevd.102.024087

published as Phys. Rev. D 102, 024087 (2020) · 18 pages, 16 figures

openalex publication_date 2020/07/30 · arxiv created 2020/08/20 · arxiv updated 2020/08/21 · openalex created_date 2022/05/11 · openalex updated_date 2026/08/06

Abstract

We continue our study of the binary neutron star parameter space by investigating the effect of the spin orientation on the dynamics, gravitational wave emission, and mass ejection during the binary neutron star coalescence. We simulate seven different configurations using multiple resolutions to allow a reasonable error assessment. Due to the particular choice of the setups, five configurations show precession effects, from which two show a precession (``wobbling'') of the orbital plane, while three show a ``bobbing'' motion; i.e., the orbital angular momentum does not precess, while the orbital plane moves along the orbital angular momentum axis. Considering the ejection of mass, we find that precessing systems can have an anisotropic mass ejection, which could lead to a final remnant kick of \ensuremath∼40 km/s for the studied systems. Furthermore, for the chosen configurations, antialigned spins lead to larger mass ejecta than aligned spins, so that brighter electromagnetic counterparts could be expected for these configurations. Finally, we compare our simulations with the precessing, tidal waveform approximant imrphenompv2_nrtidalv2 and find good agreement between the approximant and our numerical relativity waveforms with phase differences below 1.2 rad accumulated over the last \ensuremath∼16 gravitational wave cycles.

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