2003/09/30 by Masaru Shibata · 5 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.1086/377435
published as Astrophys.J.595:992,2003 · 9 pages, ApJ 595, 929 (2003)
openalex publication_date 2003/09/30 · arxiv created 2003/10/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We study the final state of the gravitational collapse of uniformly rotating supramassive neutron stars by axisymmetric simulations in full general relativity. The rotating stars provided as the initial condition are marginally stable against quasi-radial gravitational collapse, and its equatorial radius rotates with the Kepler velocity (i.e., the star is at the mass-shedding limit). To model the neutron stars, we adopt the polytropic equations of state for a wide range of the polytropic index as n = 2/3, 4/5, 1, 3/2, and 2. We follow the formation and evolution of the black holes and show that irrespective of the value of n (2/3 ≤ n ≤ 2), the final state is a Kerr black hole, and the disk mass is very small (<10 -3 of the initial stellar mass).