1997/09/30 by William G. Laarakkers, Eric Poisson · 7 citations
Engineering · Physics and Astronomy · #Angular momentum #Equation of state #Geophysics and Sensor Technology #Gravitation #Gravitational wave #Moment of inertia #Neutron star #Pulsars and Gravitational Waves Research #Quadratic equation #Quadrupole #Scientific Research and Discoveries #gr-qc
paper · pdf · doi:10.1086/306732
ReVTeX, 7 pages, 5 figures, additional material, and references added
arxiv created 1998/03/06 · openalex publication_date 1999/02/10 · arxiv updated 2015/06/25 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Numerical models of rotating neutron stars are constructed for four equations of state using the computer code RNS written by Stergioulas. For five selected values of the star's gravitational mass (in the interval between 1.0 and 1.8 solar masses) and for each equation of state, the star's angular momentum is varied from J =0 to the Keplerian limit J = J max . For each neutron star configuration, we compute Q , the quadrupole moment of the mass distribution. We show that for given values of M and J , | Q | increases with the stiffness of the equation of state. For fixed mass and equation of state, the dependence on J is well reproduced with a simple quadratic fit, Q ≃ - aJ 2 / Mc 2 , where c is the speed of light and a is a parameter of order unity depending on the mass and the equation of state.