Constraints on Neutron Star Radii Based on Chiral Effective Field Theory Interactions
K. HebelerTRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia, V6T 2A3, CanadaJames M. LattimerDepartment of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794-3800, USAC. J. PethickNORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, SwedenA. SchwenkExtreMe Matter Institute EMMI, GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
2010en
ABI
Annotatsiya
We show that microscopic calculations based on chiral effective field theory interactions constrain the properties of neutron-rich matter below nuclear densities to a much higher degree than is reflected in commonly used equations of state. Combined with observed neutron star masses, our results lead to a radius R=9.7-13.9 km for a 1.4M⊙ star, where the theoretical range is due, in about equal amounts, to uncertainties in many-body forces and to the extrapolation to high densities.
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