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Constraints from the GW170817 merger event on the nuclear matter EoS

Fiorella Burgio (Istituto Nazionale di Fisica Nucleare, Sezione di Catania, Italy)

11h00 GANIL seminar room (105)

a coffee will be served 15mn before


The equation of state (EoS) of nuclear matter is one of the key issues in understanding the physical properties of neutron stars (NS), the remnants of massive stellar collapses. Currently, the strongest constraint comes from the fact that the maximum mass for NSs must be larger than about 2 solar masses, whereas the determination of the radius is still suffering of observational uncertainties and model dependence.

Gravitational wave (GW ) observations of coalescing binary NSs have long been considered as a promising avenue to constrain the dense matter EoS. The detection of the merger event, GW170817, and its electromagnetic counterparts has put constraints on the dense matter EoS by placing lower and upper bounds on some parameters describing the binary’s tidal interactions, thus ruling out very stiff and very soft EoS. This translates into an allowed window for the radius of the 1.4Mo stellar configuration between ~11.5 and 13.5 km. Using various microscopic and phenomenological equations of state for nuclear and hybrid stars’ configurations, we find radii compatible with the
observational limits, thus identifying suitable EoS. Correlations between various observables, e.g. moment of inertia and tidal deformability, will also be discussed.

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