From Kaon-Nuclear Interactions to Kaon Condensation

Abstract

An effective chiral Lagrangian in heavy-fermion formalism whose parameters are constrained by kaon-nucleon and kaon-nuclear interactions next to the leading order in chiral expansion is used to describe kaon condensation in dense ``neutron star" matter. The critical density is found to be robust with respect to the parameters of the chiral Lagrangian and comes out to be ${\rho }_c\sim (3-4){\rho }_0$. Once kaon condensation sets in, the system is no longer composed of neutron matter but of nuclear matter. Possible consequences on stellar collapse with the formation of compact ``nuclear stars" or light-mass black holes are pointed out.

Comments: 20 pages, LaTeX, NORDITA-93/30 N, SUNY-NTG-93-7