Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 908, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/2041-8213/abdaae
Keywords
Compact objects; Neutron stars; Nuclear astrophysics; Nuclear physics; Neutron star cores; Stellar mergers; Gravitational waves
Categories
Funding
- U.S. Department of Energy, Office of Science, Office of Nuclear Physics [DE-AC52-06NA25396]
- Laboratory Directed Research and Development program of Los Alamos National Laboratory [20190617PRD1]
- U.S. Department of Energy, Office of Science, Office of Advanced Scientific Computing Research, Scientific Discovery through Advanced Computing (SciDAC) program
- research program of the Netherlands Organization for Scientific Research (NWO)
- National Science Foundation [PHY-1806990, PHY-2010970]
- CNES Postdoctoral Fellowship at Laboratoire AstroParticule et Cosmologie
- Minerva HPC cluster of the Max-PlanckInstitute for Gravitational Physics [pn56zo]
- SuperMUC-NG (LRZ) [pn56zo]
- U.S. Department of Energy National Nuclear Security Administration [89233218CNA000001]
- National Energy Research Scientific Computing Center (NERSC) - U.S. Department of Energy, Office of Science [DE-AC02-05CH11231]
- French Centre National de Recherche Scientifique (CNRS)
- Italian Istituto Nazionale della Fisica Nucleare (INFN)
- Dutch Nikhef
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The observation suggests that the compact object has a mass of 2.50-2.67M99.9%, and even with relaxed constraints on the maximum mass of neutron stars, the probability of a binary black hole origin remains around 81%. Analysis of the allowed region in the mass-radius diagram for neutron stars indicates that the scenario with a neutron star as the secondary object would require a rather stiff equation of state.
The observation of a compact object with a mass of 2.50-2.67M99.9%. Even if we weaken previously employed constraints on the maximum mass of neutron stars, the probability of a binary black hole origin is still similar to 81%. Furthermore, we study the impact that this observation has on our understanding of the nuclear equation of state by analyzing the allowed region in the mass-radius diagram of neutron stars for both a binary black hole or neutron star-black hole scenario. We find that the unlikely scenario in which the secondary object was a neutron star requires rather stiff equations of state with a maximum speed of sound c(x) >= root 0.6 times the speed of light, while the binary black hole scenario does not offer any new insight.
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