TY - JOUR
T1 - Numerical relativity simulations of prompt collapse mergers
T2 - Threshold mass and phenomenological constraints on neutron star properties after GW170817
AU - Kashyap, Rahul
AU - Das, Abhishek
AU - Radice, David
AU - Padamata, Surendra
AU - Prakash, Aviral
AU - Logoteta, Domenico
AU - Perego, Albino
AU - Godzieba, Daniel A.
AU - Bernuzzi, Sebastiano
AU - Bombaci, Ignazio
AU - Fattoyev, Farrukh J.
AU - Reed, Brendan T.
AU - Schneider, André Da Silva
N1 - Funding Information:
This research was funded by U.S. Department of Energy, Office of Science, Division of Nuclear Physics under Award No. DE-SC0021177 and by the National Science Foundation under Grants No. PHY-2011725, No. PHY-2020275, No. PHY-2116686, and No. AST-2108467. S. B. acknowledges support by the EU H2020 under ERC Starting Grant No. BinGraSp-714626. NR simulations were performed on Bridges, Comet, Stampede2 (NSF XSEDE allocation TG-PHY160025), and NSF/NCSA Blue Waters (NSF AWD-1811236) supercomputers. Computations for this research were also performed on the Pennsylvania State University’s Institute for Computational and Data Sciences’ Roar supercomputer. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Computations were also performed on the supercomputer SuperMUC-NG at the Leibniz-Rechenzentrum Munich and on the national HPE Apollo Hawk at the High Performance Computing Center Stuttgart (HLRS). The authors acknowledge the Gauss Centre for Supercomputing e.V. ( www.gauss-centre.eu ) for funding this project by providing computing time to the GCS Supercomputer SuperMUC-NG at LRZ (allocation pn68wi). The authors acknowledge HLRS for funding this project by providing access to the supercomputer HPE Apollo Hawk under the Grant No. INTRHYGUE/44215. Finally, computations were also performed on the supercomputer Joliot-Curie at GENCI@CEA and A. Perego acknowledge PRACE for awarding him access to Joliot-Curie at GENCI@CEA (PRACE Project: 2019215202).
Publisher Copyright:
© 2022 American Physical Society.
PY - 2022/5/15
Y1 - 2022/5/15
N2 - We determine the threshold mass for prompt (no bounce) black hole formation in equal-mass neutron star (NS) mergers using a new set of 227 numerical relativity simulations. We consider 23 phenomenological and microphysical finite-temperature equations of state (EOS), including models with hyperons and first-order phase transitions to deconfined quarks. We confirm the existence of EOS-insensitive relations between the threshold mass, binary tidal parameter at the threshold (Λth), maximum mass of nonrotating NSs, and radii of reference mass NSs. We combine the EOS-insensitive relations, phenomenological constraints on NS properties, and observational data from GW170817 to derive an improved lower limit on radii of maximum mass and a 1.6 M⊙ NS of 9.81 and 10.90 km, respectively. We also constrain the radius and quadrupolar tidal deformability (Λ) of a 1.4 M⊙ NS to be larger than 10.74 km and 172, respectively. We consider uncertainties in all independent parameters - fitting coefficients as well as GW170817 masses while reporting the range of radii constraints. We discuss an approach to constrain the upper as well as lower limit of NS maximum mass using future binary NS detections and their identification as prompt or delayed collapse. With future observations, it will be possible to derive even tighter constraints on the properties of matter at and above nuclear density using the method proposed in this work.
AB - We determine the threshold mass for prompt (no bounce) black hole formation in equal-mass neutron star (NS) mergers using a new set of 227 numerical relativity simulations. We consider 23 phenomenological and microphysical finite-temperature equations of state (EOS), including models with hyperons and first-order phase transitions to deconfined quarks. We confirm the existence of EOS-insensitive relations between the threshold mass, binary tidal parameter at the threshold (Λth), maximum mass of nonrotating NSs, and radii of reference mass NSs. We combine the EOS-insensitive relations, phenomenological constraints on NS properties, and observational data from GW170817 to derive an improved lower limit on radii of maximum mass and a 1.6 M⊙ NS of 9.81 and 10.90 km, respectively. We also constrain the radius and quadrupolar tidal deformability (Λ) of a 1.4 M⊙ NS to be larger than 10.74 km and 172, respectively. We consider uncertainties in all independent parameters - fitting coefficients as well as GW170817 masses while reporting the range of radii constraints. We discuss an approach to constrain the upper as well as lower limit of NS maximum mass using future binary NS detections and their identification as prompt or delayed collapse. With future observations, it will be possible to derive even tighter constraints on the properties of matter at and above nuclear density using the method proposed in this work.
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U2 - 10.1103/PhysRevD.105.103022
DO - 10.1103/PhysRevD.105.103022
M3 - Article
AN - SCOPUS:85131568986
SN - 2470-0010
VL - 105
JO - Physical Review D
JF - Physical Review D
IS - 10
M1 - 103022
ER -