Neutron matter from chiral effective field theory interactions

By Thomas Krüger, I. Tews, K. Hebeler, A. Schwenk. 2013

132 citations recorded by the source corpus.

The neutron-matter equation of state constrains the properties of many physical systems over a wide density range and can be studied systematically using chiral effective field theory (EFT). In chiral EFT, all many-body forces among neutrons are predicted to next-to-next-to-next-to-leading order (N3LO). We present details and additional results of the first complete N3LO calculation of the neutron-matter energy, which includes the subleading three-nucleon as well as the leading four-nucleon forces, and provides theoretical uncertainties. In addition, we discuss the impact of our results for astrophysics: for the supernova equation of state, the symmetry energy and its density derivative, and for the structure of neutron stars. Finally, we give a first estimate for the size of the N3LO many-body contributions to the energy of symmetric nuclear matter, which shows that their inclusion will be important in nuclear structure calculations.

View Paper: https://www.semanticscholar.org/paper/4568adc11ddfcf2a4b69ec051e2149cdee453bf7

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Citations in the corpus

• EQUATION OF STATE AND NEUTRON STAR PROPERTIES CONSTRAINED BY NUCLEAR PHYSICS AND OBSERVATION (2013, background): “In the future, these uncertainties can be reduced by improved constraints on the low-energy couplings entering 3N forces and by systematic improvements in chiral EFT that incorporate higher-order manybody forces (Tews et al. 2013; Krüger et al. 2013) and Δ degrees of freedom explicitly.”
• Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state (2017, unknown): “Between 0.6ρsat and 1.1ρsat, the EoS is well constrained by chiral effective field theory calculations (Tews et al. 2013; Hebeler et al. 2013; Krüger et al. 2013).”
• Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations (2018, unknown): “…are all found to be repulsive in PNM; (ii) the inclusion of N3LO 3N contributions does not change the repulsive nature of 3N forces in PNM, see Krüger et al. (2013) and Drischler et al. (2016); and (iii) local regulators lead to less repulsion from the 3N TPE compared to typically used…”