AI 中文总结
提出基于接触矢量流-流相互作用的单流体框架，耦合暗物质与重子物质的化学势，研究镜像暗物质对中子星状态方程、结构及冷却过程的影响。
AI 中文摘要
我们开发了一个自洽的框架，基于接触矢量流-流相互作用，通过相互平均场位移耦合两个扇区的化学势，其中暗物质（DM）分数$F_D = N_D/N_B$作为全局输入参数固定。该公式为固定密度处方提供了物理动机的替代方案，允许局部DM密度在整个恒星内部跟随重子物质（BM）密度。作为一个应用，我们考虑暗与可见扇区之间具有精确对称性的镜像DM场景，并使用NL3$\omega\rho$、FSU2R、NL3和DDME2状态方程（EOSs）研究中子星物质。我们发现DM-BM相互作用削弱了致密物质的结合，降低了其不可压缩性，并软化了EOS。因此，DM增加了中子星的中心密度和致密性，降低了其最大质量，并将直接Urca过程的起始点移至更高的恒星密度。结果，对于具有硬对称能量的模型，快速冷却的起始点移至更高质量的恒星，而对于具有软对称能量的模型，则移至更低质量的恒星，这取决于DM混合导致的额外致密性。这些结果表明，镜像DM混合改变了中子星的微观组成和宏观结构，对其热演化和多信使观测特征具有潜在影响。
英文摘要
We develop a self-consistent dark matter admix neutron star framework based on a contact vector current--current interaction that couples the chemical potentials of both sectors through mutual mean-field shifts, with the dark matter (DM) fraction $F_D = N_D/N_B$ fixed as a global input parameter. This formulation provides a physically motivated alternative to fixed-density prescriptions, allowing the local DM density to follow the baryonic matter (BM) density throughout the stellar interior. As an application, we consider a mirror-DM scenario with exact symmetry between the dark and visible sectors and investigate NS matter using the NL3$ωρ$, FSU2R, NL3, and DDME2 equations of state (EOSs). We find that the amount of DM introduced through $F_D$ weakens the binding of dense matter, reduces its incompressibility, and softens the EOS, while the DM--BM interaction governs the microscopic behavior of the DM in the dense BM medium. Consequently, DM increases the central density and compactness of NSs, lowers their maximum masses, and shifts the onset of the direct Urca process to higher stellar densities. As a consequence, the onset of rapid cooling is shifted to more massive stars for models with a stiff symmetry energy and to less massive stars for models with a soft symmetry energy, depending on the extra compactness that results from the DM admixture. These results demonstrate that mirror-DM admixtures modify both the microscopic composition and macroscopic structure of NSs, with potential implications for their thermal evolution and multimessenger observational signatures.
Comments19 pages, 9 figures, and 5 tables (Accepted for publication in Physical Review D)
