A simple model for the X-ray weakness of James Webb Space Telescope–selected broad-line active galactic nuclei (AGNs) is proposed under the assumption that the majority of these sources are fed at super-Eddington accretion rates. In these conditions, the hot inner corona above the geometrically thin disk that is responsible for the emission of X-rays in “normal” AGNs will be embedded instead in a funnel-like reflection geometry. The coronal plasma will Compton upscatter optical/UV photons from the underlying thick disk as well as the surrounding funnel walls, and the high soft-photon energy density will cool down the plasma to temperatures in the range 30–40 keV. The resulting X-ray spectra are predicted to be extremely soft, with power-law photon indices Γ ≃ 2.8–4.0, making high-z super-Eddington AGNs largely undetectable by Chandra.

中文翻译：

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X射线：从超级爱丁顿吸积到婴儿黑洞上的弱活动星系核


詹姆斯·韦伯太空望远镜选择的宽线活动星系核 （AGN） 的 X 射线弱点提出了一个简单的模型，其假设这些源中的大多数都以超爱丁顿吸积率馈送。在这些情况下，负责在“正常”AGN 中发射 X 射线的几何薄盘上方的热内日冕将被嵌入漏斗状反射几何结构中。日冕等离子体将康普顿上散射来自底层厚盘以及周围漏斗壁的光学/紫外光子，而高软光子能量密度将使等离子体冷却到 30-40 keV 范围内的温度。据预测，生成的 X 射线光谱非常柔和，幂律光子指数Γ ≃ 2.8-4.0，这使得 Chandra 基本上无法检测到高 z 超级爱丁顿 AGN。