Antikaon Condensation and In-medium Kaon and Antikaon Production in Protoneutron Stars

作     者：GU Jian-Fa GUO Hua LI Xi-Guo LIU Yu-Xin XU Fu-Rong 

作者机构：Department of Technical Physics and MOE Laboratory of Heavy Ion Physics Peking University Beijing 100871 China Center of Theoretical Nuclear Physics National Laboratory of Heavy Ion Accelerator Lanzhou 730000 China Institute of Modern Physics The Chinese Academy of Sciences Lanzhou 730000 China Department of Physics Peking University Beijing 100871 China 

出 版 物：《Communications in Theoretical Physics》 (理论物理通讯（英文版）)

年 卷 期：2007年第47卷第1期

页      面：111-118页

核心收录：

学科分类：07[理学] 070202[理学-粒子物理与原子核物理] 0702[理学-物理学] 

基　　金：The project supported by National Natural Science Foundation of China under Grant Nos. 10575005, 10275002, 10435080, 10425521, and 10135030, the Key Project of the Ministry of Education under Grant No. 305001, and the CAS Knowledge Innovation Project under Grant No. KJcx2-sw-No2 0ne of authors (Hua Guo) is indebted to Dr. S. Pal since we can check our numerical results by using his code, and also thank Dr. Z.W. Lin for his kind help 

主　　题：protoneutron stars antikaon condensation neutrino trapping 

摘      要：Antikaon condensation and kaon and antikaon production in protoneutron stars are investigated in a chiral hadronic model （also referred to as the FST model in this paper）. The effects of neutrino trapping on protoneutron stars are analyzed systematically. It is shown that neutrino trapping makes the critical density of K^- condensation delay to higher density and fifo condensation not occur. The equation of state （EOS） of （proto）neutron star matter with neutrino trapping is stiffer than that without neutrino trapping. As a result, the maximum masses of （proto）neutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are taken into account, antikaon does not form a condensate in （proto）neutron stars. Meanwhile, the corresponding EOS becomes much softer, and the maximum masses of （proto）neutron stars are smaller than those without hyprons. Finally, our results illustrate that the Q values for K^＋ and K^- production in （proto）neutron stars are not sensitive to neutrino trapping and inclusion of hyperons.