AI 中文总结
该研究用3种物态方程模型分析AMXPs结构对吸积自旋加速的影响，得到3颗AMXPs的质量约束，提出该方法可用于脉冲星状致密星质量约束，未来测量改进将完善约束。
AI 中文摘要
我们研究吸积毫秒X射线脉冲星（AMXPs）的整体结构对吸积诱导自旋加速的影响，采用3种分别代表中子星、夸克星和奇异星的物态方程（EoS）模型。通过应用经典吸积扭矩形式体系，并结合XTE J1751-305、SAX J1808.4-3658和IGR J00291+5934这3颗AMXPs的观测数据推导吸积率和磁场，我们得到了光度与自旋加速率平面内的质量等值线。结果显示，3种EoS模型推断的质量大致一致，表明该方法对特定EoS不敏感，可作为约束脉冲星状致密星质量的演化通道。值得注意的是，SAX J1808.4-3658和IGR J00291+5934被约束为极低质量，而XTE J1751-305的质量与脉冲星典型范围一致。我们的分析表明，未来距离和自旋加速测量的改进将完善这些质量约束，而使用特定EoS参数将带来新的见解。
英文摘要
We investigate the influence of the global structure of accreting millisecond X-ray pulsars (AMXPs) on accretion-induced spin-up, using three equations of state (EoS) models representing neutron stars, quark stars, and strangeon stars. By applying the classical accretion torque formalism, and deriving the accretion rate and magnetic field from observations of three AMXPs --- XTE J1751-305, SAX J1808.4-3658, and IGR J00291+5934 --- we derive mass contours in the plane of luminosity versus spin-up rate. Our results show that the inferred masses are broadly consistent across the three EoS models, indicating that the method is insensitive to the specific EoS and can serve as an evolutionary channel for constraining the masses of pulsar-like compact stars. Notably, we find that SAX J1808.4-3658 and IGR J00291+5934 are constrained to very low masses, while XTE J1751-305 yields a mass consistent with the typical range for pulsars. Our analysis suggests that future improvements in distance and spin-up measurements would refine these mass constraints, which could offer crucial evidence to distinguish different EoS models. This paper also presents the idea that using EoS-specific parameters could yield new insights.
Comments6 pages, 3 figures, 1 table
