相对论厚吸积盘的铁线轮廓和自遮蔽
Iron line profiles and self-shadowing from relativistic thick accretion discs
摘要：
我们目前的Fe K α线轮廓和图像的相对论光盘有限厚度的旋转黑洞使用一种新的代码。这条线被认为是由吸积盘最里面的一种相对冷的X射线照射物质的铁荧光产生的，它提供了对黑洞附近吸积流的极好诊断。以前的研究集中在薄的开普勒吸积盘的情况下。随着吸积率的增加，这个圆盘必须变得更厚，并且是次开普勒。这些可以影响线的轮廓，反过来又可以影响估计的吸积盘和黑洞参数从观察到的线的轮廓。我们在这里着手，第一次，一个完全相对论性的计算，提供了关键的见解的几何厚度和次开普勒轨道速度的影响的线配置文件。我们包括所有的相对论效应，如帧拖动，多普勒增强，时间膨胀，引力红移和光弯曲。我们发现，分离和相对高度之间的蓝色和红色峰值的线轮廓减小的厚度的磁盘的增加。这个代码也非常适合于产生吸积盘图像。我们计算了吸积盘的红移和通量像，发现吸积盘的观测像强烈地依赖于倾角。自遮蔽效应在大倾角时表现得很明显，并导致黑洞的阴影完全被圆盘本身所掩盖。
英文摘要：
We present Fe Kalpha line profiles from and images of relativistic discs with finite thickness around a rotating black hole using a novel code. The line is thought to be produced by iron fluorescence of a relatively cold X-ray illuminated material in the innermost parts of the accretion disc and provides an excellent diagnostic of accretion flows in the vicinity of black holes. Previous studies have concentrated on the case of a thin, Keplerian accretion disc. This disc must become thicker and sub-Keplerian with increasing accretion rates. These can affect the line profiles and in turn can influence the estimation of the accretion disc and black hole parameters from the observed line profiles. We here embark on, for the first time, a fully relativistic computation which offers key insights into the effects of geometrical thickness and the sub-Keplerian orbital velocity on the line profiles. We include all relativistic effects such as frame-dragging, Doppler boost, time dilation, gravitational redshift and light bending. We find that the separation and the relative height between the blue and red peaks of the line profile diminish as the thickness of the disc increases. This code is also well-suited to produce accretion disc images. We calculate the redshift and flux images of the accretion disc and find that the observed image of the disc strongly depends on the inclination angle. The self-shadowing effect appears remarkable for a high inclination angle, and leads to the black hole shadow being completely hidden by the disc itself.
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