发表机构
Universitat de València; Aristotle University of Thessaloniki（瓦伦西亚大学; 塞萨洛尼基亚里士多德大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究将中子星迁移测试扩展到三维旋转情形，用两种状态方程验证数值相对论代码，发现迁移后残骸近均匀旋转，并提出标准测试方法。
AI 中文摘要
在模拟动力学不稳定中子星时，截断误差可能引入扰动，驱动恒星结构要么坍缩为黑洞，要么迁移到动力学稳定、密度较低的结构。这一机制已成为验证球对称中子星模型广义相对论流体动力学代码的标准基准。在本工作中，我们将分析扩展到三维空间中演化的均匀旋转中子星这一更一般的情况。我们使用两种状态方程研究这些转变：冷多方球和混合方案，这使我们能够区分正压响应与激波产生的热压效应。我们发现迁移后的残骸在转变后保持接近均匀旋转，并通过涉及中心密度、旋转剖面和轴对称引力波通道的互补诊断追踪其准径向脉动。我们研究了这些转变的性质，并提出一个标准测试，要求迁移行为与本文报告的动力学一致，以验证数值相对论代码。
英文摘要
When simulating dynamically unstable neutron stars, truncation errors can introduce perturbations that drive the stellar configuration either toward gravitational collapse into a black hole or toward migration to a dynamically stable, lower-density configuration. This mechanism has become a standard benchmark for validating general-relativistic hydrodynamics codes in the case of spherically symmetric neutron-star models. In this work, we extend the analysis to the more general case of uniformly rotating neutron stars evolved in three spatial dimensions. We investigate these transitions using two equations of state: a cold polytrope and a hybrid prescription, which allow us to distinguish the barotropic response from the effects of shock-generated thermal pressure. We find that the migrated remnant remains close to uniform rotation after the transition, and we trace its quasi-radial pulsations through complementary diagnostics involving the central density, the rotation profile, and the axisymmetric gravitational-wave channel. We investigate the properties of these transitions and propose a standardized test for validating numerical-relativity codes by requiring the migration behavior to be consistent with the dynamics reported here.
Comments15 pages, 14 figures
