AI 中文总结
研究利用中子星相关数据约束核物质冷态方程，虽整体约束无法确定恒星核心微观组成，但超子等仍有可能。总结多信使现状，强调统一描述强相互作用物质的挑战，介绍相关成果及MUSES计算引擎的作用。
AI 中文摘要
中子星的质量、半径和旋进潮汐形变现在为冷态方程（EOS）提供了定量约束，支持在约一到两倍核饱和密度附近的相对软物质以及在更大密度下的显著变硬。然而，这些整体约束并不能唯一确定恒星核心的微观组成。超子、解禁夸克、夸克物质和强一阶相变仍然是可行的可能性。本文总结了当前的多信使状态，并强调了下一个挑战——对跨越催化中子星、双星合并和重离子碰撞的强相互作用物质进行统一描述。在SQM2026上展示的最新结果，包括对超子相互作用的新约束和多维状态方程建模的进展，突出了该计划所需的互补实验和理论输入。MUSES计算引擎提供了模块化软件基础设施，用于将这些输入与天体物理和重离子应用相连接。
英文摘要
Neutron-star masses, radii, and inspiral tidal deformabilities now provide quantitative constraints on the cold equation of state (\eos), favoring relatively soft matter around one to two times nuclear saturation density and substantial stiffening at larger density. These bulk constraints, however, do not uniquely determine the microscopic composition of the stellar core. Hyperons, deconfined quarks, quarkyonic matter, and strong first-order phase transitions remain viable possibilities. This article summarizes the present multimessenger status and emphasizes the next challenge---a unified description of strongly interacting matter across catalyzed neutron stars, binary mergers, and heavy-ion collisions. Recent results presented at SQM2026, including new constraints on hyperon interactions and advances in multidimensional equation-of-state modeling, highlight the complementary experimental and theoretical inputs required for this program. The MUSES Calculation Engine provides modular software infrastructure for connecting these inputs to astrophysical and heavy-ion applications.
CommentsSQM 2026 proceeding. 6 pages
