研究了考虑K介子凝聚的中子星物质的物态方程。此外，潮汐参数相关的二元中子星合并的组件的确定和比较的约束GW 170817对这些量。在这项研究中，我们采用最低阶约束变分（LOCV）方法，并利用{AV 6 $'$，AV 8 $'$，和AV 18势}伴随着三核子相互作用（TNI）{为了考虑核子-核子相互作用}。已知NS核中K介子的存在软化了EoS {并因此}降低了预期大于2 M $_\odot$的最大质量值。结果表明，考虑奇异值K介子凝聚时，除了AV 8 $'$ +TNI势外，$_{3}$ m $_s$ =-134 MeV满足最大质量约束.而无因次潮汐变形能力的计算表明，随着奇异度值的减小，中子星的变形变小。
英文摘要：
The equation of state (EoS) of neutron star (NS) matter is investigated considering kaon condensation. Moreover, the tidal parameters related to the components of binary neutron star mergers are determined and compared to the constraints of GW170817 imposed on these quantities. In this study, we employ the lowest-order constrained variational (LOCV) approach and utilize {AV6$'$, AV8$'$, and AV18 potentials} accompanied by the three nucleon interaction (TNI) {in order to consider the nucleon-nucleon interaction}. It is known that the existence of kaons in the core of NSs softens the EoS {and thus} lowers the value of maximum mass which is expected to be greater than 2 M$_\odot$. Our results demonstrate that considering kaon condensation with a strangeness value, a$_{3}$m$_s$=-134 MeV satisfies the maximum mass constraint except for AV8$'$+TNI potential. However, the calculation of dimensionless tidal deformability shows that with the decrease of strangeness value, the neutron star gets less deformed.
S-wave kaon condensation in neutron-star matter within a chiral model framework with dynamical meson masses
Center for Nuclear Research, Department of Physics, Kent State University（肯特州立大学核研究中心物理系）；Department of Physics, Kent State University（肯特州立大学物理系）；Department of Physics, MRPD Government College Talwara（塔尔瓦拉MRPD政府学院物理系）；Department of Physics, University of Houston（休斯顿大学物理系）；Department of Physics, Catholic Institute of Technology（天主教理工学院物理系）；Universidade Federal Fluminense（弗鲁米嫩塞联邦大学）；ICRANet（国际相对论天体物理中心网络）
Cooling of Isolated Neutron Stars with Hyperon-mixed Kaon-Condensation Matter
The University of Manchester（曼彻斯特大学）；Indian Institute of Technology, Roorkee（印度理工学院鲁尔基分校）；RIKEN（理化学研究所）；Chiba Institute of Technology（千叶工业大学）；Kurume Institute of Technology（久留米工业大学）
New equation of state involving Bose-Einstein condensate of antikaon for supernova and neutron star merger simulations
我们计算了一个新的包含$K^{-}$介子的玻色-爱因斯坦凝聚体的状态方程表，用于核塌缩、超新星和中子星合并的模拟。非均匀物质中的核和相互作用核子用一个包括排除体积效应的核统计平衡模型的扩展版本来描述，而高密度的均匀物质则用具有密度依赖耦合的相对论强子场论来处理。状态方程表是针对宽范围的密度（$10^{-12}$至$\sim 1$ fm $^{-3}$）、正电荷分数（0.01至0.60）和温度（0.1至158.48 MeV）生成的。研究了反K介子凝聚对不同热力学量，如每重子自由能、每重子熵、压强以及物质组成的影响。此外，本文还研究了反K介子凝聚的临界温度和物质的相图。
