1996/09/10 by Hideki Asada, Masaru Shibata · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.1103/physrevd.54.4944
published as Phys.Rev. D54 (1996) 4944-4954 · 25 pages including 3 tables, REVTeX, 1 postscript figure included; to appear in Physical Review D
arxiv created 1996/09/10 · openalex publication_date 1996/10/15 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present a formalism to obtain equilibrium configurations of uniformly rotating fluid in the second post-Newtonian approximation of general relativity. In our formalism, we need to solve 29 Poisson equations, but their source terms decrease rapidly enough at the external region of the matter [i.e., at worst O(r^\ensuremath-4)]. Hence these Poisson equations can be solved accurately as the boundary value problem using standard numerical methods. This formalism will be useful to obtain nonaxisymmetric uniformly rotating equilibrium configurations such as synchronized binary neutron stars just before merging and the Jacobi ellipsoid.