Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 505, Issue 2, Pages 1661-1677Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab1287
Keywords
equation of state; methods: data analysis; neutron star mergers
Categories
Funding
- European Union's H2020 under ERC Starting Grant [BinGraSp-714626]
- U.S. Department of Energy, Office of Science, Division of Nuclear Physics [DE-SC0021177]
- National Science Foundation [PHY-2011725]
- DFG [INST 275/334-1 FUGG, INST 275/363-1 FUGG]
- ERC Starting Grant [BinGraSp-714626]
- INFN
- United States National Science Foundation (NSF)
- Science and Technology Facilities Council (STFC) of the United Kingdom
- Max-Planck-Society (MPS)
- State of Niedersachsen/Germany
- Australian Research Council
- European Gravitational Observatory (EGO)
- French Centre National de Recherche Scientifique (CNRS)
- Italian Istituto Nazionale della Fisica Nucleare (INFN)
- Dutch Nikhef
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The joint detection of the binary neutron star merger on August 17, 2017, through the gravitational wave GW170817, short gamma-ray burst GRB170817A, and kilonova AT2017gfo, marks a milestone in multimessenger astronomy and provides new constraints on the neutron star equation of state. Observational data favor non-spherical geometries and multi-component models, resulting in constraints on the binary mass ratio and reduced tidal parameter. The predictions from AT2017gfo combined with those from GW170817 constrain the radius of a NS of 1.4 solar masses at 12.2 +/- 0.5 km (1 sigma level), with potential for further strengthening through improvements in kilonova models using numerical-relativity information.
The joint detection of the gravitational wave GW170817, of the short gamma-ray burst GRB170817A and of the kilonova AT2017gfo, generated by the the binary neutron star (NS) merger observed on 2017 August 17, is a milestone in multimessenger astronomy and provides new constraints on the NS equation of state. We perform Bayesian inference and model selection on AT2017gfo using semi-analytical, multicomponents models that also account for non-spherical ejecta. Observational data favour anisotropic geometries to spherically symmetric profiles, with a log-Bayes' factor of similar to 10(4), and favour multicomponent models against single-component ones. The best-fitting model is an anisotropic three-component composed of dynamical ejecta plus neutrino and viscous winds. Using the dynamical ejecta parameters inferred from the best-fitting model and numerical-relativity relations connecting the ejecta properties to the binary properties, we constrain the binary mass ratio to q < 1.54 and the reduced tidal parameter to . Finally, we combine the predictions from AT2017gfo with those from GW170817, constraining the radius of a NS of 1.4 M-circle dot to 12.2 +/- 0.5 km (1 sigma level). This prediction could be further strengthened by improving kilonova models with numerical-relativity information.
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