Kaon Condensation in Dense Stellar Matter

TL;DR

This paper explores kaon condensation in dense stellar matter using chiral perturbation theory, predicting that negatively charged kaons condense at high densities, which could lead to new phenomena in compact stars.

Contribution

It combines recent theoretical approaches and models to analyze kaon condensation, including chiral perturbation theory and Skyrme model results, providing a comprehensive view.

Findings

Kaon condensation occurs at densities 2-4 times nuclear saturation density.

Predicted kaon condensation could enable new phenomena in compact star matter.

Integrates multiple theoretical frameworks for a detailed analysis.

Abstract

This article combines two talks given by the authors and is based on works done in collaboration with G.E. Brown and D.-P. Min on kaon condensation in dense baryonic medium treated in chiral perturbation theory using heavy-baryon formalism. It contains, in addition to what was recently published, astrophysical backgrounds for kaon condensation discussed by Brown and Bethe, a discussion on a renormalization-group analysis to meson condensation worked out together with H.K. Lee and S.-J. Sin, and the recent results of K. M. Westerberg in the bound-state approach to the Skyrme model. Negatively charged kaons are predicted to condense at a critical density $2\lsim \rho/\rho_0\lsim 4$, in the range to allow the intriguing new phenomena predicted by Brown and Bethe to take place in compact star matter.