Kaon Condensation in ``Nuclear Star" Matter
arXiv:hep-ph/9403339 · doi:10.1016/0370-2693(94)90348-4
Abstract
The critical density for kaon condensation in ``nuclear star" matter is computed up to two-loop order {\it in medium} (corresponding to next-to-next-to-leading order in chiral perturbation theory in free space) with a heavy-baryon effective chiral Lagrangian whose parameters are determined from scattering and kaonic atom data. To the order considered, the kaon self-energy has highly non-linear density dependence in dense matter. We find that the four-Fermi interaction terms in the chiral Lagrangian play an important role in triggering condensation, predicting for ``natural" values of the four-Fermi interactions a rather low critical density, .
12 pages and 2 figures(LaTeX), SNUTP-94-28. The fig. 3 is replaced, with some changes in the text but the conclusion is not affected by these changes
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Cited by in corpus (14)
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- An Effective Chiral Lagrangian Approach to Kaon-Nuclear Interactions: Kaonic atom and kaon condensation
- Kaon Condensation in Dense Stellar Matter
- S-wave Meson-Nucleon Interactions and the Meson Mass in Nuclear Matter from Chiral Effective Lagrangians
- Properties of Hadrons in the Nuclear Medium
- Medium effects on the flow of strange particles in heavy ion collisions
- The Role of Lambda(1405) in Kaon-Proton Interactions
- Chiral Symmetry Restoration and the Georgi Vector Limit
- Chiral Perturbation Theory in a Nuclear Background
- Renormalization-Group Flow Analysis of Meson Condensations in Dense Matter
- Energy level displacement of excited np states of kaonic hydrogen
- On radiative np -> 1s + gamma transitions, induced by strong low-energy interactions,in kaonic atoms