标题： 中子星状态方程的观测探针：超子、玻色子暗物质和夸克物质 显示英文标题

标题： Observational Probes of the Neutron Star Equation of State with Hyperons, Bosonic Dark Matter, and Quark Matter

摘要： 暗物质在中子星中的存在由于其可能对中子星结构和可观测特性的影响而日益受到关注。 在提出的候选粒子中，假设的六夸克粒子已作为有前景的玻色子暗物质粒子出现，可能在中子星核心的极端条件下形成。 我们使用相对论密度泛函方法研究了这一情景，包括超子（DD2Y-T模型）用于强子相，并与由非局部Nambu-Jona-Lasinio模型描述的禁闭夸克相耦合。 通过平滑的交叉过渡来模拟相变，并通过有效质量位移引入六夸克-重子相互作用，以表示排斥作用。 我们评估了这种混合情景，包括超子、玻色子暗物质和禁闭夸克物质，是否符合中子星的多信使约束。 通过扫描参数空间，我们确定了与质量半径测量和潮汐变形性一致的六夸克质量。 我们的结果表明，六夸克的存在会软化状态方程，使模型能够在典型$1.4M_\odot$中子星周围满足半径和潮汐变形性约束。 我们包含了所有可用的NICER数据，包括PSR J0437-4715和新发布的PSR J0614-3329。 我们发现，六夸克质量接近1900 MeV的混合星符合所有当前观测限制，包括HESS J1731-347和PSR J0952-0607，代表了最轻和最重的已知中子星。 此外，我们进行了贝叶斯分析，得出的 favored 六夸克质量范围为1885-1935 MeV，支持这种奇异粒子在中子星内部的潜在作用。 显示英文摘要

摘要： The presence of dark matter in neutron stars is of growing interest due to its possible impact on their structure and observables. Among proposed candidates, the hypothetical sexaquark has emerged as a promising bosonic dark matter particle, potentially forming under extreme conditions in neutron star cores. We investigate this scenario using a relativistic density functional approach, including hyperons (DD2Y-T model) for the hadronic phase, coupled to a deconfined quark phase described by a non-local Nambu-Jona-Lasinio model. The phase transition is modeled through a smooth crossover, and sexaquark-baryon interactions are introduced via an effective mass shift representing repulsion. We assess whether this hybrid scenario, incorporating hyperons, bosonic dark matter, and deconfined quark matter, is consistent with multi-messenger constraints from neutron stars. By scanning the parameter space, we identify sexaquark masses that are consistent with mass-radius measurements and tidal deformability. Our results show that the presence of the sexaquark softens the equation of state, enabling the model to satisfy both the radius and tidal deformability constraints around the canonical $1.4M_\odot$ neutron stars. We incorporate all available NICER data, including PSR J0437-4715 and newly published PSR J0614-3329. We find out that hybrid stars with sexaquark mass near 1900 MeV agree with all current observational limits, including HESS J1731-347 and PSR J0952-0607, representing the lightest and most massive known neutron stars. Furthermore, we perform a Bayesian analysis, which yields a favored sexaquark mass range of 1885-1935 MeV, supporting the potential role of this exotic particle in the interiors of neutron stars.