利用XRISM/Resolve对Cen X-3掩食进入和离开阶段的光谱分析

中文摘要 AI 辅助

我们利用XRISM/Resolve的高分辨率光谱，以两个掩食外区间作为参考，研究了高质量X射线双星Cen X-3在掩食进入和离开阶段的分相位X射线光谱演化，以约束吸收物质和Fe K发射区。我们使用SPEX对光谱进行建模，包括星际和本地风吸收、幂律和黑体连续谱、盘反射以及Fe XXV和Fe XXVI的高斯分量。我们将吸收柱密度的轨道变化与平滑的CAK风模型进行比较，并研究Fe Kα谱线宽度的变化。本地吸收柱密度变化了近两个数量级，从掩食前的N_H^local = 4.25 x 10^22 cm^-2变化到掩食时的5.9 x 10^23 cm^-2。仅靠平滑风模型无法再现掩食时过量的吸收，这表明视线方向上存在局部过密结构。Fe Kα谱线宽度从掩食前的约510 km s^-1变化到掩食离开时的1400 km s^-1，而在掩食进入和掩食后阶段，其值约为900 km s^-1，且在统计上无法区分。在整个轨道上都探测到了高度电离的Fe XXV和Fe XXVI发射，尽管在掩食进入阶段分辨出的分量较少。这些诊断揭示了一个复杂的星周环境，其中包含局部致密物质和多个再处理区域。这些结果展示了XRISM/Resolve探测掩食高质量X射线双星中吸积环境几何结构和运动学的能力。

英文摘要

We investigate the phase-resolved X-ray spectral evolution of the high-mass X-ray binary Cen X-3 across eclipse ingress and egress, using two out-of-eclipse intervals as references, to constrain the absorbing material and Fe K emitting regions with high-resolution XRISM/Resolve spectroscopy. We model the spectra with SPEX, including interstellar and local wind absorption, a power-law and blackbody continuum, disk reflection, and Gaussian components for Fe XXV and Fe XXVI. We compare the orbital variation of the absorbing column with a smooth CAK wind model and investigate the variability of the Fe K alpha line width. The local absorbing column varies by nearly two orders of magnitude, from N_H^local = 4.25 x 10^22 cm^-2 during pre-ingress to 5.9 x 10^23 cm^-2 at ingress. The excess ingress absorption cannot be reproduced by a smooth wind model alone, suggesting a localized overdense structure along the line of sight. The Fe K alpha width varies from approximately 510 km s^-1 during pre-ingress to 1400 km s^-1 during egress, with intermediate, statistically indistinguishable values of approximately 900 km s^-1 during ingress and post-egress. Highly ionized Fe XXV and Fe XXVI emission is detected throughout the orbit, although fewer components are resolved during ingress. These diagnostics reveal a complex circumstellar environment with localized dense material and multiple reprocessing regions. The results demonstrate the capability of XRISM/Resolve to probe the geometry and kinematics of accretion environments in eclipsing high-mass X-ray binaries.

发表机构

• Universidad de Alicante（阿利坎特大学）
• SRON Space Research Organisation Netherlands（荷兰空间研究组织）
• NASA/Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
• The University of Tokyo（东京大学）
• Japan Aerospace Exploration Agency (JAXA)（日本宇宙航空研究开发机构）
• University of Maryland, College Park（马里兰大学帕克分校）
• Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·范·伦斯贝赫天体物理研究所）

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