前中子星内的K-凝聚和超子的生成

用相对论平均场下的手征强子模型研究了前中子星内K^-凝聚和超子的生成。结果显示，前中子星内的中微子束缚使得出现K^-凝聚的临界密度推迟到更高的重子密度，而K^-0凝聚无法出现。同时中微子束缚使得前中子星的状态方程变硬，从而前中子星的最大质量变大。如果考虑超子，前中子星内无法出现K^-凝聚，同时系统的状态方程变软（与不含超子的情况相比），从而对应前中子星的最大质量变小。A chiral hadronic model is extended to investigate antikaon condensation and hyperons production of protoneutron stars. Our results show that neutrino trapping makes the critical density of K^- condensation delay to higher density and K^-0 condensation not occur. Meanwhile, the equation of state （EOS） of （proto）neutron star matter considering neutrino trapping is stiffer than the case without neutrino trapping. Therefore the maximum masses of rotoneutron stars with neutrino trapping are larger than those without neutrino trapping. If hyperons are considered, antikaon condensation does not appear 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.

Antikaon Condensation and Hyperons Production in Protoneutron Stars

A chiral hadronic model is extended to investigate antikaon condensation and hyperons production of protoneutron stars.Our results show that neutrino trapping makes the critical density of K~-condensation delay to higher density and ~0 condensation not occur.Meanwhile,the equation of state(EOS) of(proto)neutron star matter considering neutrino trapping is stiffer than the case without neutrino trapping.Therefore the maximum masses of protoneutron stars with neutrino trapping are larger than those without neutrino trapping.If hyperons are considered,antikaon condensation does not appear 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.