XRB、AGN和ULX的硬X射线谱演化
The Hard X-ray Spectral Evolution in XRBs, AGNs and ULXs
摘要：
我们探讨了硬X射线光子指数$Γ$和爱丁顿比（$Γ$ = L_{X}（0.5-25 keV）/ L_{Edd}）之间的关系。我们发现，当$ξ$小于某一临界值时，不同的XRB在$Γ$和$ξ$之间遵循不同的反相关性，而当$ξ$大于该临界值时，它们遵循相同的正相关性。这种反相关和正相关在LLAGN和类星体中也分别存在，并且不同XRB的反相关和正相关大致收敛到同一点（$\log ξ=-2.1, Γ=1.5$），这可能对应于吸积模的转变，因为反相关和正相关分别与ADAF和标准盘/日冕系统的预测相一致。传统的低/硬状态被交叉点$\log ξ\sim-2.1$分为两部分，即，反相关部分为弱硬状态，正相关部分为亮硬状态。在硬亮态下的吸积过程可能仍然是高软态下的标准吸积盘，这与在某些硬亮态下观察到的冷盘成分和宽的Fe K发射线相一致。ADAF仅在弱硬态XRB中重要。激发的ULXs的XRB的状态转换和定时属性的相似性，我们然后约束BH质量为7发光ULXs假设他们的X射线光谱演化是类似的XRB。我们发现这7个ULX的BH质量都在$10^{4}M_sun$附近，是典型的中等质量BH（IMBH）。我们的结果与从模型拟合多色盘和/或定时属性（例如，QPO和中断频率）。
英文摘要：
We explore the relationship between the hard X-ray photon index $Γ$ and the Eddington ratio (ξ=L_{X}(0.5-25 keV)/L_{Edd}) in six XRBs. We find that different XRBs follow different anti-correlations between $Γ$ and $ξ$ when $ξ$ is less than a critical value, while they follow the same positive correlation when $ξ$ is larger than the critical value. This anti-correlation and positive correlation are also found in LLAGNs and QSOs respectively, and the anti-correlation and positive correlation of different XRBs roughly converge to the same point ($\log ξ=-2.1, Γ=1.5$), which may correspond to the accretion mode transition, since that the anti-correlation and positive correlation are consistent with the prediction of ADAFs and standard disk/corona system respectively. The traditional low/hard state are divided into two parts by the cross point $\log ξ\sim-2.1$, i.e., faint-hard state in the anti-correlation part and bright-hard state in the positive correlation part. The accretion process in the bright-hard state may be still the standard accretion disk as that in the high/soft state, which is consistent with that both the cold disk component and broad Fe K emission line are observed in some bright-hard state of XRBs. The ADAF is only important in the faint-hard state XRBs. Motivated by the similarities of the state transition and timing properties of the ULXs to that of XRBs, we then constrain the BH masses for seven luminous ULXs assuming that their X-ray spectral evolution is similar to that of XRBs. We find that the BH masses of these seven ULXs are around $10^{4}M_sun$, which are typical intermediate mass BHs (IMBHs). Our results are roughly consistent with the BH masses constrained from the model fitting with a multi-color disk and/or the timing properties(e.g., QPO and break frequency).
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