In this work, we construct a sample of black hole X‐ray binaries (BH XRBs), low‐luminosity active galactic nuclei (LLAGNs), and FR Is with wider distribution of Eddington ratios and re‐explore their fundamental plane of BH activities, that is, . We find that the quiescent BH sources follow a similar fundamental plane (ξ_X ∼ 0.6) with sub‐Eddington BH sources very well, while the strong radio sources (e.g., FR Is) follow a steeper fundamental plane (ξ_X ∼ 1.30). We also find that the radio–X‐ray correlation of quiescent BH sources are still on the extension of sub‐Eddington BH sources and the strong radio sources follow a steeper correlation (ξ_X ∼ 1.30). The results are consistent with recent observations in BH XRBs. It is predicted that the X‐ray emissions of both sub‐Eddington BH sources and quiescent BH sources originate from radiatively inefficient accretion mode, while the X‐ray emissions of strong radio sources dominantly originate from the jet.

中文翻译：

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静态源黑洞活动的基本平面

在这项工作中，我们构造了一个黑洞X射线双星（BH XRB），低发光活性银河核（LLAGNs）和FR Is样本，这些样本具有更大的爱丁顿比分布，并重新探究了它们的BH活动基本面，即。我们发现，静态BH来源遵循类似的基本面（ξ _X  〜0.6与子爱丁顿BH源）非常出色，而强大的射电源（例如，FR是）遵循一个陡峭的基本面（ξ _X  〜1.30）。我们还发现，静态工作BH源无线电X射线的相关性仍然在分爱丁顿BH源的扩展性和强大的射电源遵循一个陡峭的相关性（ξ _X  〜1.30）。结果与最近在BH XRB中的观察结果一致。可以预言，亚爱丁顿BH源和静态BH源的X​​射线辐射都来自辐射效率低下的积聚模式，而强无线电源的X射线辐射主要来自射流。