论文标题
kaon-baryon耦合方案和高音混合物中的kaon冷凝
Kaon-baryon coupling schemes and kaon condensation in hyperon-mixed matter
论文作者
论文摘要
根据相对论的均值场理论与有效的手性lagrangian相结合，研究了高度致密物质（（$ y+k $）阶段（$ y+k $）阶段[（$ y+k $）阶段]中的可能共存。比较了$ s $ - 波量kaon-baryon的两个耦合方案，在超音混音物质中的kaon凝结的开始密度和已发达的状态方程（$ y+k $）阶段：一个是与非线性有效的chiral lagral lagral lagral lagral lagral lagrangian相关的状态（$ y+k $）阶段。另一个是介子 - 交换方案，其中通过交换介子（Sigma，Sigma，Sigma^* Mesons用于标量耦合）以及Omega，Rho，Rho，Phi Mesons，用于矢量耦合）。结果表明，在梅森交换方案中，非线性标量自我相互作用的贡献产生了KAON有效能量的排斥作用，与接触交互方案相比，提高了KAON凝结的开始密度。通常，接触相互作用方案和介子交换方案之间的kaon-baryon动力学差异取决于非线性自我相互作用的介子项的特定形式。结果表明，非线性的自我相互作用项与排斥能量无关，导致状态方程在高密度下的僵硬，并且由于接触交互方案的情况下（$ y $+$ k $）阶段（$ y $+$ k $）阶段的出现，它不能用大量的吸引力来补偿。我们还在接触相互作用方案中讨论哪种效果是必要的，以使状态方程（y+k）相足够僵硬，以与最近对大型中子星的观察结果保持一致。
Possible coexistence of kaon condensation and hyperons in highly dense matter [the ($Y+K$) phase] is investigated on the basis of the relativistic mean-field theory combined with the effective chiral Lagrangian. Two coupling schemes for the $s$-wave kaon-baryon interaction are compared regarding the onset density of kaon condensation in the hyperon-mixed matter and equation of state for the developed ($Y+K$) phase: One is the contact interaction scheme related to the nonlinear effective chiral Lagrangian. The other is the meson-exchange scheme, where the interaction vertices between the kaon field and baryons are described by exchange of mesons (sigma, sigma^* mesons for scalar coupling, and omega, rho, phi mesons for vector coupling). It is shown that in the meson exchange scheme, the contribution from the nonlinear scalar self-interaction gives rise to a repulsive effect for kaon effective energy, pushing up the onset density of kaon condensation as compared with the case of the contact interaction scheme. In general, the difference of kaon-baryon dynamics between the contact interaction scheme and the meson-exchange scheme relies on the specific forms of the nonlinear self-interacting meson terms. It is shown that the nonlinear self-interacting term is not relevant to repulsive energy leading to stiffening of the equation of state at high densities and that it cannot be compensated with large attractive energy due to the appearance of the ($Y$+$K$) phase in the case of the contact interaction scheme. We also discuss in the contact interaction scheme what effects are necessary so as to make the equation of state with (Y+K) phase stiff enough to be consistent with recent observations of massive neutron stars.
