The chiral condensate in neutron matter

Abstract

We calculate the chiral condensate in neutron matter at zero temperature based on nuclear forces derived within chiral effective field theory. Two-, three- and four-nucleon interactions are included consistently to next-to-next-to-next-to-leading order (N3LO) of the chiral expansion. We find that the interaction contributions lead to a modest increase of the condensate, thus impeding the restoration of chiral symmetry in dense matter and making a chiral phase transition in neutron-rich matter unlikely for densities that are not significantly higher than nuclear saturation density.

arXiv commentpublished version, 6 pages, 4 figures

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Cited by in corpus (14)

• From hadrons to quarks in neutron stars: a review
• Roy-Steiner-equation analysis of pion-nucleon scattering
• Functional renormalization group studies of nuclear and neutron matter
• From asymmetric nuclear matter to neutron stars: a functional renormalization group study
• The QCD Axion at Finite Density
• Functional renormalization group approach to neutron matter
• To which densities is spin-polarized neutron matter a weakly interacting Fermi gas?
• Pi in the Sky: Neutron Stars with Exceptionally Light QCD Axions
• Relativistic self-energy decomposition of nuclear symmetry energy and equation of state of neutron matter within QCD sum rules
• From QCD Symmetries to Nuclei and Neutron Stars
• Dense Baryonic Matter and Strangeness in Neutron Stars
• Neutron matter within QCD sum rules
• Single-Particle Spectrum of Pure Neutron Matter
• Partial restoration of chiral symmetry in hot and dense neutron matter