Physics

Energy (signal processing)

Isoscalar

Isovector

RADIUS

Nuclear matter

Nucleon

Dark energy

Nuclear physics

Neutron star

Cosmology

Dense matter

Computer science

Astrophysics

Star (game theory)

Quantum mechanics

Quintessence

Computer security

Equation of state

Physical review. C

Constraints set on key parameters of the nuclear matter equation of state (EoS) by the values of the tidal deformability, inferred from GW170817, are examined by using a diverse set of relativistic and nonrelativistic mean-field models. These models are consistent with bulk properties of finite nuclei as well as with the observed lower bound on the maximum mass of neutron star $\ensuremath{\approx}2{M}_{\ensuremath{\bigodot}}$. The tidal deformability shows a strong correlation with specific linear combinations of the isoscalar and isovector nuclear matter parameters associated with the EoS. Such correlations suggest that a precise value of the tidal deformability can put tight bounds on several EoS parameters, in particular on the slope of the incompressibility and the curvature of the symmetry energy. The tidal deformability obtained from the GW170817 and its UV, optical and infrared counterpart sets the radius of a canonical $1.4{M}_{\ensuremath{\bigodot}}$ neutron star to be $11.82\ensuremath{\le}{R}_{1.4}\ensuremath{\le}13.72\phantom{\rule{4pt}{0ex}}\mathrm{km}$.

GW170817: Constraining the nuclear matter equation of state from the neutron star tidal deformability