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An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers
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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 $1.4M_\odot$ neutron star to be $R=11.98^{+0.35}_{-0.40}$km.
Forward citations
Cited by 7 Pith papers
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Binary neutron stars in the next-generation era: Multi-messenger detection prospects and constraints on the equation of state, mass distribution, and cosmology
With ET (and ET+CE), mock multi-messenger BNS catalogues yield ~40–500 EM counterparts per year and, under ideal recovery, constrain R1.4 to ~0.2 km and H0 to ~1 km s−1 Mpc−1.
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nmma: An extended Bayesian framework for Nuclear Multimessenger Astronomy in the Era of Next-Generation Detectors
nmma now jointly samples nuclear EoS parameters with GW and EM data via TOV emulators and Fiesta surrogates, delivering 20–60× speedups and future H0–nuclear constraints.
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Bayesian analysis of properties of nuclear matter with the FOPI experimental data
Bayesian fits to FOPI Au+Au flow and stopping data yield m*/m0 around 0.78-0.88 and F around 0.75-0.88, while K0 remains unconstrained.
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Inferring neutron star merger ejecta morphologies with kilonovae
Kilonova ejecta morphology is distinguishable only when late-time JWST mid-infrared data are added to Rubin optical data, and AT2017gfo is best matched by the SuperNu TP2 (toroidal plus peanut wind) model.
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Prospect of Constraining the EoS of Neutron Stars Using Post-Merger Signals
Combining BAYESTACK radius posteriors for four masses through a common piecewise-polytrope EoS forecasts ~1 km (uniform prior) or ~0.55 km (astrophysical prior) radius constraints from A+ era post-merger signals.
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Microscopic constraints for the equation of state and structure of neutron stars: a Bayesian model mixing framework
A Bayesian model mixing framework using Gaussian processes extends chiral EFT and pQCD constraints to neutron star matter and demonstrates kernel-dependent equation of state and mass-radius predictions.
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Toward a Unified Understanding of the Dense Matter Equation of State
A review of three Bayesian/computational frameworks for combining heavy-ion and astrophysical constraints on the dense-matter equation of state, plus a proposed unified integration workflow.
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