Functional renormalization group studies of nuclear and neutron matter

TL;DR

This paper reviews the application of functional renormalization group methods to nuclear and neutron matter, highlighting how fluctuations beyond mean-field improve the understanding of phase transitions, equations of state, and chiral symmetry restoration in dense matter.

Contribution

It introduces a FRG approach based on a chiral Lagrangian for nuclear matter, incorporating fluctuations beyond mean-field, and compares results with ab-initio calculations and perturbative methods.

Findings

Equations of state agree with advanced many-body computations.

Chiral symmetry remains broken up to high densities with fluctuations included.

Neutron star matter constraints are discussed in the context of two-solar-mass stars.

Abstract

Functional renormalization group (FRG) methods applied to calculations of isospin-symmetric and asymmetric nuclear matter as well as neutron matter are reviewed. The approach is based on a chiral Lagrangian expressed in terms of nucleon and meson degrees of freedom as appropriate for the hadronic phase of QCD with spontaneously broken chiral symmetry. Fluctuations beyond mean-field approximation are treated solving Wetterich's FRG flow equations. Nuclear thermodynamics and the nuclear liquid-gas phase transition are investigated in detail, both in symmetric matter and as a function of the proton fraction in asymmetric matter. The equations of state at zero temperature of symmetric nuclear matter and pure neutron matter are found to be in good agreement with advanced ab-initio many-body computations. Contacts with perturbative many-body approaches (in-medium chiral perturbation theory) are discussed. As an interesting test case, the density dependence of the pion mass in the medium is investigated. The question of chiral symmetry restoration in nuclear and neutron matter is addressed. A stabilization of the phase with spontaneously broken chiral symmetry is found to persist up to high baryon densities once fluctuations beyond mean-field are included. Neutron star matter including beta equilibrium is discussed under the aspect of the constraints imposed by the existence of two-solar-mass neutron stars.