Microscopic chiral-EFT equation of state for beta-stable neutron matter yields tidal deformability values inside GW170817 bounds and excludes stiff EOS with radii above ~13 km.
Cui,et al., Constraint on the symmetry energy at high density from neutron star observations using relativistic mean- field models, Nuclear Science and Techniques 36 (2025) 141
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Tidal deformability in neutron stars from a microscopic point of view
Microscopic chiral-EFT equation of state for beta-stable neutron matter yields tidal deformability values inside GW170817 bounds and excludes stiff EOS with radii above ~13 km.