An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers

Peter T. H. Pang, Tim Dietrich (), Michael W. Coughlin, Mattia Bulla, Ingo Tews, Mouza Almualla, Tyler Barna, Ramodgwendé Weizmann Kiendrebeogo, Nina Kunert, Gargi Mansingh, Brandon Reed, Niharika Sravan, Andrew Toivonen, Sarah Antier, Robert O. VandenBerg, Jack Heinzel, Vsevolod Nedora, Pouyan Salehi, Ritwik Sharma, Rahul Somasundaram and Chris Van Den Broeck
Additional contact information
Peter T. H. Pang: Nikhef
Tim Dietrich: Universität Potsdam
Michael W. Coughlin: University of Minnesota
Mattia Bulla: Stockholm University, AlbaNova
Ingo Tews: Los Alamos National Laboratory
Mouza Almualla: American University of Sharjah
Tyler Barna: University of Minnesota
Ramodgwendé Weizmann Kiendrebeogo: Université Joseph KI-ZERBO
Nina Kunert: Universität Potsdam
Gargi Mansingh: University of Minnesota
Brandon Reed: University of Minnesota
Niharika Sravan: Drexel University
Andrew Toivonen: University of Minnesota
Sarah Antier: Université Côte d’Azur, CNRS
Robert O. VandenBerg: University of Minnesota
Jack Heinzel: Massachusetts Institute of Technology
Vsevolod Nedora: Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
Pouyan Salehi: Universität Potsdam
Ritwik Sharma: University of Delhi
Rahul Somasundaram: Los Alamos National Laboratory
Chris Van Den Broeck: Nikhef

Nature Communications, 2023, vol. 14, issue 1, 1-13

Abstract: Abstract The multi-messenger detection of the gravitational-wave signal GW170817, the corresponding kilonova AT2017gfo and the short gamma-ray burst GRB170817A, as well as the observed afterglow has delivered a scientific breakthrough. For an accurate interpretation of all these different messengers, one requires robust theoretical models that describe the emitted gravitational-wave, the electromagnetic emission, and dense matter reliably. In addition, one needs efficient and accurate computational tools to ensure a correct cross-correlation between the models and the observational data. For this purpose, we have developed the Nuclear-physics and Multi-Messenger Astrophysics framework NMMA. The code allows incorporation of nuclear-physics constraints at low densities as well as X-ray and radio observations of isolated neutron stars. In previous works, the NMMA code has allowed us to constrain the equation of state of supranuclear dense matter, to measure the Hubble constant, and to compare dense-matter physics probed in neutron-star mergers and in heavy-ion collisions, and to classify electromagnetic observations and perform model selection. Here, we show an extension of the NMMA code as a first attempt of analyzing the gravitational-wave signal, the kilonova, and the gamma-ray burst afterglow simultaneously. Incorporating all available information, we estimate the radius of a 1.4M⊙ neutron star to be $$R=11.9{8}_{-0.40}^{+0.35}$$ R = 11.9 8 − 0.40 + 0.35 km.

Date: 2023
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DOI: 10.1038/s41467-023-43932-6

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