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#### Binary Neutron Stars with Arbitrary Spins in Numerical Relativity

##### MPG-Autoren
/persons/resource/persons145564

Haas,  Roland
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Ossokine,  Serguei
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

##### Externe Ressourcen
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##### Volltexte (frei zugänglich)

1508.06986.pdf
(Preprint), 3MB

PhysRevD.92.124012.pdf
(beliebiger Volltext), 3MB

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##### Zitation

Tacik, N., Foucart, F., Pfeiffer, H. P., Haas, R., Ossokine, S., Kaplan, J., et al. (2015). Binary Neutron Stars with Arbitrary Spins in Numerical Relativity. Physical Review D, 92: 124012. doi:10.1103/PhysRevD.92.124012.

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 quasi-local angular momentum integrals. When constructing irrotational binary neutron stars, we find a very small residual dimensionless spin of $\sim 2\times 10^{-4}$. 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 $\sim 0.1\%$. The neutron stars show quasi-normal mode oscillations at an amplitude which increases with the rotation rate of the stars.