STOKES 表与 KY 代码
STOKES tables and KY codes
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中文总结 AI 辅助
本文介绍了与 XSPEC 兼容的全相对论 KY 代码系列，该代码采用 STOKES 生成的预计算表，可对 X 射线双星和活动星系核进行光谱-偏振建模，并提供了拟合 IXPE 数据的示例及代码仓库链接。
中文摘要 AI 辅助
KY 代码系列是一款与 XSPEC 兼容的全相对论模型包，用于 X 射线双星系统和活动星系核的光谱-偏振建模。在克尔时空内，它们计算吸积盘的线轮廓、康普顿化冕辐射照射下的盘反射光谱，以及包含盘-冕相互作用和盘自辐照的热盘发射。这些模型中许多包含偏振计算，更高级的时序变体可计算 X 射线、紫外和光学混响。康普顿化 X 射线的主要源被假设为在盘几何结构上方的 lamp-post 共轴区域或平板中。KY 代码以不同复杂度运行：一些模型使用局域再处理的解析近似，另一些则依赖详细的数值表。为了对部分电离吸积盘大气中的静止帧再处理进行最精确处理，KY 代码采用用 STOKES 代码生成的预计算光谱-偏振表。这些透射和反射表也设计为可在 XSPEC 中独立使用，并作为 KY 之外更高级模型的输入。本章首先介绍各种变体的 STOKES 表，展示它们在 XSPEC 模型中的非相对论用法，用于两种场景：（i）扩展源照射遥远的几何薄盘；（ii）致密源照射垂直延展的赤道遮挡物（如环面或厚风）。随后描述相对论 KY 光线追踪，再介绍每个 KY 模型，还展示了使用这些模型对 X 射线双星和活动星系核的 IXPE 数据进行拟合的示例。这些模型共同构成了一个全面且公开可用的吸积光谱-偏振建模与数据拟合框架，我们提供了其在线代码仓库的链接。
英文摘要
The family of KY codes is an XSPEC-compatible package of fully relativistic models for spectro-polarimetric modeling of X-ray binary systems and active galactic nuclei. Within Kerr space-time, they compute accretion disc line profiles, reflection spectra from discs illuminated by Comptonized coronal radiation, and thermal disc emission including disc-corona interaction and disc self-irradiation. Many of these models include polarimetric computations, and more advanced timing variants compute X-ray, UV and optical reverberation. The primary source of Comptonized X-rays is assumed to be in the lamp-post on-axis or slab above the disc geometry. The KY codes operate at various levels of complexity; some models use analytical approximations for local re-processing, while others rely on detailed numerical tables. For the most accurate treatment of rest-frame re-processing in partially ionized accretion disc atmospheres, the KY codes employ pre-computed spectro-polarimetric tables generated with the STOKES code. These transmission and reflection tables are also designed for standalone use in XSPEC and as inputs to higher-level models beyond KY. The chapter first introduces the STOKES tables in various variants and shows their non-relativistic usage in XSPEC models for (i) an extended source illuminating a distant geometrically thin disc, and (ii) a compact source illuminating a vertically extended equatorial obscurer (e.g., a torus or thick wind). The relativistic KY ray-tracing is then described, followed by an introduction to each KY model. Examples of fits to the IXPE data of X-ray binaries and active galactic nuclei using these models are shown. Together, these models form a comprehensive and publicly available framework for spectro-polarimetric modeling and data fitting of accretion. We provide links to their online repositories.
发表机构
- Astronomical Institute of the Czech Academy of Sciences（捷克科学院天文研究所）
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