AI 中文总结
本研究构建含超子反应的自洽反应网络，发现双中子星并合时奇异粒子输运呈代数衰减，增强体粘滞并产生可探测的引力波相移，为探测中子星内部超子提供新手段。
AI 中文摘要
中子星核心中超子的存在会开启快速的奇异粒子平衡通道，在双中子星并合过程中产生体粘滞耗散。由于这些反应与电子β平衡共存，潮汐压缩可驱动这两种耦合的化学失衡远超出线性响应范围。我们构建了首个反应网络，该网络结合四维奇异粒子依赖的手征平均场（CMF）物态方程，自洽演化电子和奇异粒子分数，包含核子与超子的URCA过程以及非轻子超子反应。针对代表并合振荡的周期性密度扰动，我们发现快速奇异粒子转化可产生大的β失衡，随后缓慢的β平衡会成为奇异粒子弛豫的瓶颈。因此耦合系统在远离平衡态下呈现出具有动力学重要性的代数衰减，而非指数衰减。在并合过程预期的keV温度下，这种非线性响应使有效体粘滞显著增强，对于320Hz振荡可达约10³¹ g·cm⁻¹·s⁻¹。对持续并合耗散的唯象估计显示，具有超子核心的中子星的引力波相移可达约0.14弧度。因此自洽的、远离平衡态的奇异粒子输运可作为探测中子星内部超子的动力学探针。
英文摘要
The presence of hyperons in the cores of neutron stars opens fast strangeness equilibration channels that can produce bulk-viscous dissipation during binary inspiral. Because these reactions coexist with electron $β$-equilibration, tidal compression can drive the two coupled chemical imbalances far beyond linear response. We construct the first reaction network that self-consistently evolves the electron and strangeness fractions with a four-dimensional strangeness-dependent chiral mean-field (CMF) equation of state, including nucleonic and hyperonic Urca processes and non-leptonic hyperon reactions. For periodic density perturbations, representative of inspiral oscillations, we find that rapid strangeness conversion can generate a large $β$-imbalance, after which slow $β$-equilibration bottlenecks strangeness relaxation. Rather than decaying exponentially, the coupled system consequently exhibits dynamically important algebraic decay in a far-from-equilibrium regime. At the $\rm keV$ temperatures expected during inspiral, this nonlinear response produces a broad enhancement of the effective bulk viscosity, reaching $\sim10^{31}\,\mathrm{g\,cm^{-1}\,s^{-1}}$ for $320$ Hz oscillations. A phenomenological estimate of continuous inspiral dissipation yields gravitational-wave phase shifts up to $\sim0.14$ rad for neutron stars with hyperonic cores. Self-consistent, far-from-equilibrium strangeness transport may therefore provide a dynamical probe of hyperons in neutron-star interiors.
Comments21 pages, 10 figures
