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The radius of a typical-mass neutron star and chiral effective field theory

Research paper by Francesca Sammarruca, Randy Millerson

Indexed on: 04 Mar '18Published on: 04 Mar '18Published in: arXiv - Nuclear Theory



Abstract

We calculate neutron star masses and radii from equations of state based on chiral few-nucleon interactions at third and fourth order of the chiral expansion. Our focus is on the radius of a 1.4 M_Sun neutron star, which we discuss in relation to the pressure in neutron-rich matter at normal density. Our predictions for the radius are consistent with the most recent constraints. We also show the full M(R) relations up to their respective maximum masses. Beyond the densities for which we have derived microscopic predictions from chiral forces, the equations of state are obtained via polytropic continuations.