1998/09/18 by Stuart L. Shapiro · 2 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Gamma-ray bursts and supernovae #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.1103/physrevd.58.103002
published as Phys.Rev. D58 (1998) 103002 · to appear in Physical Review D (revtex, 3 figs, 5 pgs)
arxiv created 1998/09/18 · openalex publication_date 1998/10/08 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The head-on collision of identical neutron stars from rest at infinity requires a numerical simulation in full general relativity for a complete solution. Undaunted, we provide a relativistic, analytic argument to suggest that during the collision, sufficient thermal pressure is always generated to support the hot remnant in quasi-static stable equilibrium against collapse prior to slow cooling via neutrino emission. Our conclusion is independent of the total mass of the progenitors and holds even if the remnant greatly exceeds the maximum mass of a cold neutron star.