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.
Koehn,et al., From existing and new nuclear and astrophysical constraints to stringent limits on the equation of state of neutron-rich dense matter, Phys
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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.