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We explore constraints on the equation of state (EOS) of neutron-rich matterbased on microscopic calculations up to nuclear densities and observations ofneutron stars. In a previous work we showed that predictions based on modernnuclear interactions derived within chiral effective field theory and theobservation of two-solar-mass neutron stars result in a robust uncertaintyrange for neutron star radii and the EOS over a wide range of densities. Inthis work we extend this study, employing both the piecewise polytropeextension from Hebeler et al. as well as the speed of sound model of Greif etal., and show that moment of inertia measurements of neutron stars cansignificantly improve the constraints on the EOS and neutron star radii.

Equation of state constraints from nuclear physics, neutron star masses, and future moment of inertia measurements