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

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In this paper, 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.
Abstract
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.

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Journal ArticleDOI

GW170817: Measurements of Neutron Star Radii and Equation of State.

B. P. Abbott, +1238 more
TL;DR: This analysis expands upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars.
Journal ArticleDOI

Gravitational-wave constraints on the neutron-star-matter Equation of State

TL;DR: It is concluded 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_{⊙})=120.4%.
Journal ArticleDOI

New Constraints on Radii and Tidal Deformabilities of Neutron Stars from GW170817.

TL;DR: A parameterized manner a very large range of physically plausible equations of state (EOSs) for compact stars for matter that is either purely hadronic or that exhibits a phase transition is explored, finding the radius that is statistically most probable for any value of the stellar mass.
Journal ArticleDOI

From hadrons to quarks in neutron stars: a review.

TL;DR: In this article, the authors describe the structure of neutron stars constructed from the unified equations of states with crossover, and present the current equations of state-called "QHC18" for quark-hadron crossover-in a parametrized form practical for neutron star modeling.
Journal ArticleDOI

Neutron Skins and Neutron Stars in the Multimessenger Era

TL;DR: Ab et al. as mentioned in this paper used a set of realistic models of the equation of state (EOS) that yield an accurate description of the properties of finite nuclei, support neutron stars of two solar masses, and provide a Lorentz covariant extrapolation to dense matter are used to confront its predictions against gravitational-wave data.
References
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Journal ArticleDOI

GW170817: observation of gravitational waves from a binary neutron star inspiral

B. P. Abbott, +1134 more
TL;DR: The association of GRB 170817A, detected by Fermi-GBM 1.7 s after the coalescence, corroborates the hypothesis of a neutron star merger and provides the first direct evidence of a link between these mergers and short γ-ray bursts.
Journal ArticleDOI

Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A

B. P. Abbott, +1198 more
TL;DR: In this paper, the authors used the observed time delay of $(+1.74\pm 0.05)\,{\rm{s}}$ between GRB 170817A and GW170817 to constrain the difference between the speed of gravity and speed of light to be between $-3
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