Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State.

By Eemeli Annala, Tyler Gorda, A. Kurkela, A. Vuorinen. Physical Review Letters, 2017

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The detection of gravitational waves originating from a neutron-star merger, GW170817, by the LIGO and Virgo Collaborations has recently provided new stringent limits on the tidal deformabilities of the stars involved in the collision. Combining this measurement with the existence of two-solar-mass stars, we generate a generic family of neutron-star-matter equations of state (EOSs) that interpolate between state-of-the-art theoretical results at low and high baryon density. Comparing the results to ones obtained without the tidal-deformability constraint, we witness a dramatic reduction in the family of allowed EOSs. Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that the smallest allowed tidal deformability of a similar-mass star is Λ(1.4 M_{⊙})=120.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/08a569ccd9cd03033997c8312863b58ccb773e05

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Citations in the corpus

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].”
A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation (2019, methodology): “These can be translated, usually by means of universal relations or EOS model assumptions, into constraints on mass and radius (see, e.g., Abbott et al. 2018; Annala et al. 2018; De et al. 2018; Most et al. 2018; Tews et al. 2018b).”
A NICER View of PSR J0030+0451: Implications for the Dense Matter Equation of State (2019, background): “Independent analyses of GW170817-only data (De et al. 2018) and results (e.g., Annala et al. 2018; Lim & Holt 2018; Most et al. 2018; Raithel et al. 2018; Tews et al. 2018b) obtained compatible constraints of the radius in a broad range of Rä[9, 14] km.”
Constraining the Dense Matter Equation of State with Joint Analysis of NICER and LIGO/Virgo Measurements (2019, result): “The results were consistent, leading to R = 11.9+1.4−1.4 km from the spectral EOS analysis and R = 10.8+2.0−1.7 km for the more massive NS at the 90% credible interval (Abbott et al. 2018); see also De et al. (2018); Annala et al. (2018); Tews et al. (2018) for independent related work.”
Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations (2018, methodology): “For studies using different models for the high-density EOS constrained by chiral interactions at low densities, please see Annala et al. (2018), Most et al. (2018), and Lim & Holt (2018).”
Equation of state sensitivities when inferring neutron star and dense matter properties (2018, background): “…properties from observational data, including gravitational wave observations of neutron star mergers like GW170817 (Abbott et al. 2017), see e.g. Abbott et al. (2018), Annala et al. (2018), Most et al. (2018), Tews, Margueron & Reddy (2018a), and Lim & Holt (2018) that use parametrized EOS models.”