Abstract
We discuss the constraints on the equation of state (EOS) of neutron star matter obtained by the data analysis of the neutron star-neutron star merger in the event GW170807. To this scope, we consider two recent microscopic EOS models computed starting from two-body and three-body nuclear interactions derived using chiral perturbation theory. For comparison, we also use three representative phenomenological EOS models derived within the relativistic mean field approach. For each model, we determine the β -stable EOS and then the corresponding neutron star structure by solving the equations of hydrostatic equilibrium in general relativity. In addition, we calculate the tidal deformability parameters for the two neutron stars and discuss the results of our calculations in connection with the constraints obtained from the gravitational wave signal in GW170817. We find that the tidal deformabilities and radii for the binary’s component neutron stars in GW170817, calculated using a recent microscopic EOS model proposed by the present authors, are in very good agreement with those derived by gravitational waves data.
Highlights
The physics of neutron stars represents a way to test our understanding of matter under extreme conditions of density and temperature
We have studied how recent estimates of the tidal deformabilities of the binary’s component neutron stars, obtained by the analysis of the gravitational waves (GW) data in the event GW170817, can help to constrain the equation of state (EOS) of neutron star matter
We have considered some microscopic and phenomenological EOS models for nucleonic as well as hyperonic matter
Summary
The physics of neutron stars represents a way to test our understanding of matter under extreme conditions of density and temperature. Large variation of the density in the range ∼10 × 1015 g/cm are expected in neutron stars This requires the modeling of systems in very different physical conditions such as heavy neutron rich nuclei arranged to form a lattice structure as in the outer crust of the star, or a charge neutral system of interacting hadrons (nucleons, and possibly hyperons or a phase with deconfined quarks) and leptons forming a quantum fluid as in the stellar core [1]. The description of such a variety of systems, of considerable interest for nuclear physics as well as for astrophysics, needs for a challenging theoretical effort and an accurate knowledge of the interactions between the particles present inside the star. Approach with the aim of comparing with the results obtained using microscopic EOS models
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