Fe Kα PROFILES FROM SIMULATIONS OF ACCRETING BLACK HOLES
Fe Kα PROFILES FROM SIMULATIONS OF ACCRETING BLACK HOLES
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黑洞吸积模拟中的 Fe Kα 分布
DOI：
10.3847/0004-637x/826/1/52
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
J. Krolik
中科院分区：
文献类型：
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作者：
B. Kinch;J. Schnittman;T. Kallman;J. Krolik
我们展示了直接从广义相对论磁流体动力学 (GRMHD) 模拟预测 Fe Kα 剖面的新技术的第一个结果。 GRMHD 模拟的数据由蒙特卡罗全局辐射传输代码处理，该代码自洽地确定了照射盘表面的 X 射线通量和日冕电子温度。利用从模拟中得出的辐射通量和圆盘的密度结构，我们从光电离平衡和辐射传输方程的解中确定了再处理的 Fe Kα 发射。我们制作了磁盘表面 Fe Kα 发射的表面亮度图，对于我们以爱丁顿值 1% 吸积的史瓦西黑洞为例，其在最内层稳定圆形轨道半径之外急剧上升一个引力半径，然后在更大的半径处下降 ∝r−2。我们将 Fe Kα 径向表面亮度分布的这些特征分别解释为圆盘电离结构和扩展日冕几何形状的结果。我们还展示了相应的 Fe Kα 线轮廓，如远处观察者在几种倾角下所看到的。线轮廓的形状和我们预测的 Kα 线的等效宽度在质量上与通常从吸积黑洞中观察到的相似。最重要的是，这项工作代表了理论和观测之间的直接联系：以完全自洽的方式，我们从黑洞吸积理论中产生了可观测的结果——铁荧光线轮廓，几乎没有现象学假设。
We present the first results from a new technique for the prediction of Fe Kα profiles directly from general relativistic magnetohydrodynamic (GRMHD) simulations. Data from a GRMHD simulation are processed by a Monte Carlo global radiation transport code, which determines the X-ray flux irradiating the disk surface and the coronal electron temperature self-consistently. With that irradiating flux and the disk’s density structure drawn from the simulation, we determine the reprocessed Fe Kα emission from photoionization equilibrium and solution of the radiation transfer equation. We produce maps of the surface brightness of Fe Kα emission over the disk surface, which—for our example of a Schwarzschild black hole accreting at 1% the Eddington value—rises steeply one gravitational radius outside the radius of the innermost stable circular orbit and then falls ∝r−2 at larger radii. We explain these features of the Fe Kα radial surface brightness profile as consequences of the disk’s ionization structure and an extended coronal geometry, respectively. We also present the corresponding Fe Kα line profiles as would be seen by distant observers at several inclinations. Both the shapes of the line profiles and the equivalent widths of our predicted Kα lines are qualitatively similar to those typically observed from accreting black holes. Most importantly, this work represents a direct link between theory and observation: in a fully self-consistent way, we produce observable results—iron fluorescence line profiles—from the theory of black hole accretion with almost no phenomenological assumptions.
DOI：
10.1088/0004-637x/720/1/205
发表时间：
2009-08
期刊：
The Astrophysical Journal
影响因子：
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作者：
E. Cackett
通讯作者：
E. Cackett