2012/09/12 by Wolfgang Tichy · 2 citations
Mathematics · Physics and Astronomy · #Angular velocity #Astro and Planetary Science #Astrophysics #Binary number #Binary star #Classical mechanics #Compressibility #Conservative vector field #Gamma-ray bursts and supernovae #Geometry #Mathematics #Mechanics #Neutron star #Newtonian fluid #Physics #Pulsars and Gravitational Waves Research #Rotation (mathematics) #Spins #Stars #Stellar rotation #astro-ph.SR #gr-qc
paper · pdf · doi:10.1103/physrevd.86.064024
published as Phys. Rev. D 86, 064024 (2012) · fixed typos in Eq. (27), 8 pages, 3 figures
openalex publication_date 2012/09/12 · arxiv created 2014/11/04 · arxiv updated 2015/06/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In general neutron stars in binaries are spinning. Recently, a new quasi-equilibrium approximation that includes a rotational velocity piece for each star has been proposed to describe binary neutron stars with arbitrary rotation states in quasicircular orbits. We have implemented this approximation numerically for the first time, to generate initial data for neutron star binaries with spin. If we choose the rotational velocity piece such that it equals the Newtonian rigid rotation law, we obtain stars with fluid 4-velocities that have expansion and shear of approximately zero, as one would expect for quasi-equilibrium configurations. We also use the new approach to construct and study initial data sequences for irrotational, corotating, and fixed rotation binaries.