GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations

By David Radice, Albino Perego, F. Zappa, Sebastiano Bernuzzi. 2017

517 citations recorded by the source corpus.

Gravitational waves detected from the binary neutron star (NS) merger GW170817 constrained the NS equation of state by placing an upper bound on certain parameters, describing the binary’s tidal interactions. We show that the interpretation of the UV/optical/infrared counterpart of GW170817 with kilonova models, combined with new numerical-relativity results, imply a complementary lower bound on the tidal deformability parameter. The joint constraints tentatively rule out both extremely stiff and soft NS equations of state.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c1845f212e1d3b9c729693b88f29b15758946c9b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, background): “…observation of the NS-NS merger GW170817 (Abbott et al. 2017) marks the dawn of a new era in probing NS physics with gravitational waves, and it is already providing new insights on the EoS (Annala et al. 2017; Banik & Bandyopadhyay 2017; Radice et al. 2018; Most et al. 2018; Zhang et al. 2018).”
A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, methodology): “While this process has been modeled as local “effective viscosity” (e.g., Radice et al. 2018; Shibata et al. 2017), angular momentum redistribution could in principle be dominated by torques from large-scale magnetic fields, even if they are weaker in magnitude than the smallerscale turbulent ones.”
Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, unknown): “(Radice et al. 2018) for a very recent review.”
From hadrons to quarks in neutron stars: a review (2017, methodology): “The event has also been used to place constraints on the radii of the initial neutron stars [161], as well as to suggest a lower bound on the tidal deformability of the stars [162].”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “Recently, the observation of gravitational waves from the merger of a binary system of neutron stars also allowed to put stringent constraints upon the EOS of matter at supranuclear densities [33, 182, 183].”
Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations (2018, methodology): “…the source properties of GW170817 and EOS with statistical methods modelling the light curve and spectra of AT2017gfo with surrogate models of radiative transfer simulations [see e.g. Bauswein et al. (2017); Radice et al. (2018) for alternative approaches combining EM and GW information].”
Critical examination of constraints on the equation of state of dense matter obtained from GW170817 (2018, unknown): “5 1.8 2.0 2.2 2.4 2.6 2.8 3.0 Mmax [Msol] 100 200 300 400 500 600 700 Λ̃ ntr = 0.32fm −3 q = 1 q = 0.7 Margalit et al. (2017) Rezzolla et al. (2018) Shibata et al. (2017) Radice et al. (2018) FIG.”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, methodology): “Indeed, while viscosity impacts the overall ejecta mass (Table 2 and Radice et al. 2018b), it does not affect the electron fraction and the isotopic abundances of the r-process in the dynamical ejecta.”