*EXTRAORDINARIO: notar lugar, día y hora*. Neutron Star Equation of State after the GW170817 event"

In this talk I will review the method of estimation of tidal
deformabilities of compact stars and present results for pure hadronic
as well as hybrid stars that include the mass twins case. Then I will
discuss the impact of the nuclear symmetry energy in
the determination of the compact star radius. In particular, the recent
detection of gravitational radiation from the GW170817 event
shed light on the properties of the neutron star equation of state (EoS),
thus comprising both the study of the symmetry energy
and stellar radius. Furthermore, I shall address the question of the
possibility of a universal symmetry energy contribution to
the neutron star equation of state under restricted Direct Urca cooling.
When these two aspects are combined, powerful predictions for the
stiffness of the neutron star EoS are obtained.

Furthermore, I will focus on the case of mass twin compact stars, hybrid
compact stars with approximately the same masses but different radii.
To qualify the above, I will show a recent developed EoS that features of
a color superconducting chiral quark model with nonlocal, covariant
interactions bearing density dependent vector meson coupling and a
density-dependent bag pressure. This model allows for a scenario where the
compact stars of the GW170817 event are either both hadronic, both hybrid,
or simultaneously hadronic and hybrid configurations.