Mass of charged pions in neutron-star matter

We examine the behavior of charged pions in neutron-rich matter using heavy-baryon chiral perturbation theory. This study is motivated by the prospect that pions, or pionlike excitations, may be relevant in neutron-rich matter encountered in core-collapse supernovae and neutron star mergers. We find, as previously expected, that the n-mass increases with density and precludes s-wave condensation at nB <= nsat, where nsat approximate to 0.16 fm-3 is the nuclear saturation density, and the mass of the n+ mode decreases with density. The uncertainty in these predictions increases rapidly for nB >= nsat because low-energy constants associated with the two-pion-twonucleon operators in chiral perturbation theory are poorly constrained. These uncertainties are especially large in symmetric nuclear matter and should be included in the analysis of pion-nucleus interactions at low-energy and pionic atoms. In neutron-rich matter, accounting for the self-energy difference between neutrons and protons related to the nuclear symmetry energy has several effects. It alters the power counting of certain higher-order contributions to the pion self-energy. Previously unimportant but attractive diagrams are enhanced, resulting in a modest reduction of the pion masses. Furthermore, in the long-wavelength limit, a collective mode with the quantum numbers of the n+ appears.