用随机扰动吸积盘模型解释活动星系核双峰发射线的变化
Interpreting the Variability of Double-Peaked Emission Lines in Active Galactic Nuclei with Stochastically Perturbed Accretion Disk Models
摘要：
为了解释某些活动星系核宽双峰轮廓的短时标变化，我们构造了随机扰动的吸积盘模型，计算了亮斑旋转、剪切和衰变时的H α线轮廓序列。我们确定的依赖性的属性的线轮廓的变化对点的属性。我们比较了从模型中观察到的Arp 102 B和3C 390.3的H α线的变异性。我们发现，斑点需要集中在线发射区域的外部，以再现所观察到的Arp 102 B的可变性。这排除了恒星/盘碰撞产生的斑点，并有利于边缘自引力半径在线发射区域内的情况，从而在外部产生径向斑点分布的急剧增加。在3C 390.3的情况下，我们测试的所有模型系列都可以重现观察到的变异性，以选择合适的模型参数。
英文摘要：
In an effort to explain the short-timescale variability of the broad, double-peaked profiles of some active galactic nuclei, we constructed stochastically perturbed accretion disk models and calculated H alpha line profile series as the bright spots rotate, shear and decay. We determined the dependence of the properties of the line profile variability on the spot properties. We compared the variability of the line profile from the models to the observed variability of the H alpha line of Arp 102B and 3C 390.3. We find that spots need to be concentrated in the outer parts of the line emitting region to reproduce the observed variability properties for Arp 102B. This rules out spot production by star/disk collisions and favors a scenario where the radius of marginal self-gravity is within the line emitting region, creating a sharp increase in the radial spot distribution in the outer parts. In the case of 3C 390.3, all the families of models that we tested can reproduce the observed variability for a suitable choice of model parameters.
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