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

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.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-D7D0-C Version Permalink: http://hdl.handle.net/21.11116/0000-0006-D7D4-8
Genre: Journal Article

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 Creators:
Chaurasia, Swami Vivekanandji, Author
Dietrich, Tim, Author
Ujevic, Maximiliano, Author
Hendriks, Kai, Author
Dudi, Reetika1, Author              
Fabbri, Francesco Maria, Author
Tichy, Wolfgang, Author
Brügmann, Bernd, Author
Affiliations:
1Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 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.

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 Dates: 2020-03-262020-04-012020
 Publication Status: Published in print
 Pages: 17 pages, 15 figures
 Publishing info: -
 Table of Contents: -
 Rev. Type: -
 Identifiers: arXiv: 2003.11901
DOI: 10.1103/PhysRevD.102.024087
URI: http://arxiv.org/abs/2003.11901
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Title: Physical Review D
Source Genre: Journal
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Pages: - Volume / Issue: 102 (2) Sequence Number: 024087 Start / End Page: - Identifier: -