Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
By C. Capano, I. Tews, S. M. Brown, B. Margalit, S. De, Sumit Kumar, Duncan A. Brown, B. Krishnan, S. Reddy. Nature Astronomy, 2019
362 citations recorded by the source corpus.
The properties of neutron stars are determined by the nature of the matter that they contain. These properties can be constrained by measurements of the star’s size. We obtain stringent constraints on neutron-star radii by combining multimessenger observations of the binary neutron-star merger GW170817 with nuclear theory that best accounts for density-dependent uncertainties in the equation of state. We construct equations of state constrained by chiral effective field theory and marginalize over these using the gravitational-wave observations. Combining this with the electromagnetic observations of the merger remnant that imply the presence of a short-lived hypermassive neutron star, we find that the radius of a 1.4 M ⊙ neutron star is $${R}_{1.4{M}_{\odot }}={11.0}_{-0.6}^{+0.9}\ {\rm{km}}$$ R 1.4 M ⊙ = 11.0 − 0.6 + 0.9 km (90% credible interval). Using this constraint, we show that neutron stars are unlikely to be disrupted in neutron star–black hole mergers; subsequently, such events will not produce observable electromagnetic emission. The combination of electromagnetic and gravitational-wave observations of binary neutron-star merger GW170817 with systematic sets of neutron-star equations of state has produced a tightly constrained radius of 11 km for a 1.4 M ⊙ neutron star. This constraint suggests that a neutron star–black hole merger is unlikely to produce an electromagnetic counterpart.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/9db5719ae6fa826010ab1110ed6daf3ecf36c800
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In Astronomy and Astrophysics
Citations in the corpus
- Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, background): “of canonical NSs are approximately mass independent [13,98,106].”
- On the Sound Speed in Neutron Stars (2022, background): “4< 13.45 km) and slightly larger, but well within the error bars of the estimates by Huth et al. (2021; see also Abbott et al. 2018; Radice & Dai 2019; Capano et al. 2020; Dietrich et al. 2020; Biswas et al. 2021, for similar estimates).”
- Constraining the Dense Matter Equation of State with Joint Analysis of NICER and LIGO/Virgo Measurements (2019, methodology): “Capano et al. (2020) used a different speed of sound parameterization based on similar chiral EFT constraints, as well as different priors, in particular a uniform distribution in radius.”