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

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##### Citation

Chaurasia, S. V., Dietrich, T., Ujevic, M., Hendriks, K., Dudi, R., Fabbri, F. M., et al. (2020).
Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the spin orientation.*
Physical Review D,* *102*(2): 024087. doi:10.1103/PhysRevD.102.024087.

Cite as: https://hdl.handle.net/21.11116/0000-0006-D7D0-C

##### 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 about $\sim 40 \rm km/s$ for the studied

systems. Furthermore, for the chosen configurations, anti-aligned 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 $\sim$ 16 gravitational wave cycles.

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 about $\sim 40 \rm km/s$ for the studied

systems. Furthermore, for the chosen configurations, anti-aligned 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 $\sim$ 16 gravitational wave cycles.