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We examine possibilities of pion condensation with zero momentum (s-wavecondensation) in neutron stars by using the pion-nucleus optical potential Uand the relativistic mean field (RMF) models. We use low-densityphenomenological optical potentials parameterized to fit deeply bound pionicatoms or pion-nucleus elastic scatterings. Proton fraction (Y_p) and electronchemical 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 starsand especially has no chance if hyperons appear in neutron star matter and/orb_1 parameter in U has density dependence.

Possibility of s-wave pion condensates in neutron stars revisited