The chiral condensate in neutron matter
arXiv:1307.2110 · doi:10.1016/j.physletb.2013.08.022
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.
published version, 6 pages, 4 figures
References in corpus (12)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- The Nuclear Equation of State and Neutron Star Masses
- Neutron matter at next-to-next-to-next-to-leading order in chiral effective field theory
- Constraints on neutron star radii based on chiral effective field theory interactions
- Three-body forces: From cold atoms to nuclei
- Signals of the QCD phase transition in core-collapse supernovae
- Improving the convergence of the chiral expansion for nuclear forces II: low phases and the deuteron
- In-medium chiral condensate beyond linear density approximation
- Baryon masses, chiral extrapolations, and all that
- Chiral condensate in neutron matter
- The chiral quark condensate and pion decay constant in nuclear matter at next-to-leading order
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