2012/08/31 by Vasileios Paschalidis, Z. B. Etienne, Zachariah B. Etienne +1 · 79 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Equation of state #Gamma-ray bursts and supernovae #Gravitational collapse #Gravitational wave #Mechanics #Neutron star #Numerical relativity #Physics #Pulsars and Gravitational Waves Research #Thermodynamics #astro-ph.HE #astro-ph.SR #gr-qc
paper · pdf · doi:10.1103/physrevd.86.064032
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 86(6) (American Physical Society) · 13 pages, 7 figures, matches published version
arxiv created 2012/09/18 · openalex publication_date 2012/09/18 · arxiv updated 2012/09/19 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The inspiral and merger of a binary neutron star (NSNS) can lead to the formation of a hypermassive neutron star (HMNS). As the HMNS loses thermal pressure due to neutrino cooling and/or centrifugal support due to gravitational wave emission, and/or magnetic breaking of differential rotation, it will collapse to a black hole. To assess the importance of shock-induced thermal pressure and cooling, we adopt an idealized equation of state and perform NSNS simulations in full general relativity through late inspiral, merger, and HMNS formation, accounting for cooling. We show that thermal pressure contributes significantly to the support of the HMNS against collapse and that thermal cooling accelerates its ``delayed'' collapse. Our simulations demonstrate explicitly that cooling can induce the catastrophic collapse of a hot hypermassive neutron star formed following the merger of binary neutron stars. Thus, cooling physics is important to include in NSNS merger calculations to accurately determine the lifetime of the HMNS remnant and to extract information about the neutron star equation of state, cooling mechanisms, bar instabilities and B-fields from the gravitational waves emitted during the transient phase prior to black hole formation.