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arXiv 0705.1374astro-ph
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用软X射线谱估算黑洞质量

Black hole mass estimates from soft X-ray spectra

R. Soria, Z. Kuncic

备注：
14 pages, accepted for publication on Advances in Space Research. Based on work presented at the 2006 Cospar Scientific Assembly
发表信息：
Adv.Space Res.42:517-522,2008
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摘要：

在没有直接运动学测量的情况下，吸积黑洞的质量有时可以从其吸积盘的X射线光谱参数中推断出来;具体地说，可以从盘-黑体模型拟合的温度和归一化中推断出来。当吸积速率接近或超过爱丁顿极限时，必须引入适当的修正。我们总结的唯象模型，可以解释非常高的状态，明显较高的磁盘温度和较低的内部磁盘半径。相反，超铝X射线源通常包含具有大特征半径的较冷盘。我们为这种吸积状态引入另一种唯象模型。我们认为，一个标准盘主导的辐射输出半径大于一个特征过渡半径R_c ~ mdot × R_{ISCO}，其中mdot是在爱丁顿单位和R_{ISCO}是最内的稳定轨道的吸积率。当R_{ISCO} < R < R_c时，大部分吸积功率是通过非热过程释放的。我们预测的位置，这样的来源在光度-温度图。我们的结论是，质量约50-100 Msun的黑洞在mdot ~ 10-20吸积可以解释许多ULX的X射线性质。

英文摘要：

In the absence of direct kinematic measurements, the mass of an accreting black hole is sometimes inferred from the X-ray spectral parameters of its accretion disk; specifically, from the temperature and normalization of a disk-blackbody model fit. Suitable corrections have to be introduced when the accretion rate approaches or exceeds the Eddington limit. We summarize phenomenological models that can explain the very high state, with apparently higher disk temperatures and lower inner-disk radii. Conversely, ultraluminous X-ray sources often contain cooler disks with large characteristic radii. We introduce another phenomenological model for this accretion state. We argue that a standard disk dominates the radiative output for radii larger than a characteristic transition radius R_c ~ mdot x R_{ISCO}, where mdot is the accretion rate in Eddington units and R_{ISCO} is the innermost stable orbit. For R_{ISCO} < R < R_c, most of the accretion power is released via non-thermal processes. We predict the location of such sources in a luminosity-temperature plot. We conclude that black holes with masses ~ 50-100 Msun accreting at mdot ~ 10-20 may explain the X-ray properties of many ULXs.

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