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Constraints on Microscopic and Phenomenological Equations of State of Dense Matter from GW170817

1
Dipartimento di Fisica, Universitá di Pisa, Largo Bruno Pontecorvo 3, I-56127 Pisa, Italy
2
INFN, Sezione di Pisa, Largo Bruno Pontecorvo 3, I-56127 Pisa, Italy
*
Author to whom correspondence should be addressed.
Universe 2019, 5(10), 204; https://doi.org/10.3390/universe5100204
Received: 23 July 2019 / Revised: 18 September 2019 / Accepted: 23 September 2019 / Published: 25 September 2019
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. View Full-Text
Keywords: neutron stars; neutron star mergers; gravitational waves; equation of state neutron stars; neutron star mergers; gravitational waves; equation of state
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Logoteta, D.; Bombaci, I. Constraints on Microscopic and Phenomenological Equations of State of Dense Matter from GW170817. Universe 2019, 5, 204.

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