发表机构
Scuola Universitaria Superiore IUSS Pavia; Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica (INAF)（帕维亚高等大学学院; 布拉耶天文台，意大利国家天体物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究对比牛顿与相对论性吸积盘模型拟合软态天鹅座X-1的朱雀数据，发现牛顿内半径支持高自旋克尔轨道，相对论模型未普遍更优，张力源于数据简并而非广义相对论失效。
AI 中文摘要
软态天鹅座X-1的热连续谱通常使用牛顿时空近似下的多色盘模型进行拟合。这一选择便于估算内半径，但忽略了黑洞附近的相对论效应；这些效应通常通过颜色修正和边界条件因子来恢复。利用一次典型观测的朱雀卫星数据，我们在保持吸收、电离风、康普顿化和反射处理相同的情况下，将该牛顿描述与若干完全相对论性盘模型进行比较。在质量、距离和倾角固定为当前最佳动力学值的情况下，牛顿内半径与高自旋克尔最内层稳定圆轨道一致。相对论性模型并未提供对光谱的一致更优描述：部分模型使拟合变差或使自旋、倾角和硬化参数不受约束，而形式上最佳的模型要求倾角远大于动力学值或自旋较小。模型与数据之间的明显张力源于数据简并和有限能带，而非广义相对论的失效。
英文摘要
The thermal continuum of Cygnus X-1 in the soft state is often modelled with a multicolour disc in a Newtonian spacetime approximation. That choice is convenient for estimating the inner radius, but it neglects relativistic effects near the black hole; these are usually restored through colour-correction and boundary-condition factors. Using Suzaku data from one exemplary observation, we compare this Newtonian description with some fully relativistic disc models, keeping the same treatment of absorption, ionised winds, Comptonization and reflection. With the mass, distance and inclination fixed to the best current dynamical values, the Newtonian inner radius is consistent with a high-spin Kerr innermost stable circular orbit. The relativistic models do not provide a uniformly better description of the spectrum: some worsen the fit or leave spin, inclination and hardening unconstrained, while the formally best model requires an inclination much larger than the dynamical one or a smaller spin. Apparent tensions with the models arise from data degeneracies and from the limited energy band, not from a failure of general relativity.
Comments11 pages, 1 figure, 5 tables
