arXiv:0810.3531·v2·Nuclear Theory
Possibility of s-wave pion condensates in neutron stars revisited
A. Ohnishi (1) · D. Jido (1) · T. Sekihara (2) · K. Tsubakihara (3) ((1) YITP, Kyoto Univ., (2) Dept. of Phys., Kyoto Univ., (3) Dept. of Phys., Hokkaido Univ.)
Abstract
We examine possibilities of pion condensation with zero momentum (s-wave condensation) in neutron stars by using the pion-nucleus optical potential U and the relativistic mean field (RMF) models. We use low-density phenomenological optical potentials parameterized to fit deeply bound pionic atoms or pion-nucleus elastic scatterings. Proton fraction (Y_p) and electron chemical potential (mu_e) in neutron star matter are evaluated in RMF models. We find that the s-wave pion condensation hardly takes place in neutron stars and especially has no chance if hyperons appear in neutron star matter and/or b_1 parameter in U has density dependence.
Comments: 4 pages, 3 figures, REVTeX