The study of hadron properties in dense medium created in relativistic heavy ion collision is a subject of considerable current interest. Of particular importance is the in-medium modification of kaon properties. The ...The study of hadron properties in dense medium created in relativistic heavy ion collision is a subject of considerable current interest. Of particular importance is the in-medium modification of kaon properties. The knowledge is useful for our understanding of both chiral symmetry restoration in dense matter and the properties of the dense nuclear matter existing in neutron stars.展开更多
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 protone...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.展开更多
The K<SUP>?</SUP> nucleus differential elastic scattering cross section for <SUP>12</SUP>C and <SUP>40</SUP>Ca at is calculated with three momentum-dependent optical potential mode...The K<SUP>?</SUP> nucleus differential elastic scattering cross section for <SUP>12</SUP>C and <SUP>40</SUP>Ca at is calculated with three momentum-dependent optical potential models, which are density-dependent, relativistic mean field, and hybrid model, respectively. It is found that the forms of momentum-dependent optical potential models proposed by us are reasonable and gain success in the calculations and the momentum-dependent hybrid model is the best model for the K<SUP>?</SUP> nucleus elastic scattering.展开更多
基金Supported by the CAS knowledge innovation project ( No.KJcx2-sw-N02) and Ministry of Science and Technology of the People's Republic of China (No. 2002ccb00200).
文摘The study of hadron properties in dense medium created in relativistic heavy ion collision is a subject of considerable current interest. Of particular importance is the in-medium modification of kaon properties. The knowledge is useful for our understanding of both chiral symmetry restoration in dense matter and the properties of the dense nuclear matter existing in neutron stars.
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.
文摘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.
文摘The K<SUP>?</SUP> nucleus differential elastic scattering cross section for <SUP>12</SUP>C and <SUP>40</SUP>Ca at is calculated with three momentum-dependent optical potential models, which are density-dependent, relativistic mean field, and hybrid model, respectively. It is found that the forms of momentum-dependent optical potential models proposed by us are reasonable and gain success in the calculations and the momentum-dependent hybrid model is the best model for the K<SUP>?</SUP> nucleus elastic scattering.
