1995-2007年3C 390.3的光谱光学监测：II。谱线参数的变异性
Spectral optical monitoring of 3C 390.3 in 1995-2007: II. Variability of the spectral line parameters
摘要：
研究了具有双峰发射线轮廓的活动星系3C390.3的宽发射线参数的变化。我们给出了一个详细的分析，在广泛的Ha和Hb的配置文件，比率，和不同线段的巴耳末减量的变化。研究的线轮廓的变化，我们探索的磁盘结构，这是假设发射宽双峰Ha和Hb发射线。我们将观测到的光谱分为两个时期（2002年爆发前和爆发后），分别分析了这两个时期的变化。首先，我们分析了Ha和Hb的光谱发射线轮廓，测量峰位置。然后，我们把线分成几段，我们测量线段通量。总Ha和Hb通量，以及线段的巴耳末减量变化进行了研究和讨论。我们用一个吸积盘模型来模拟线参数的变化。我们比较了所观察到的线参数与磁盘模型预测的变化，发现线轮廓和线段的变化对应于盘状BLR的发射。但是，也可能有一个额外的排放成分，有助于Ha和Hb线中心。我们发现，谱线轮廓的变化是由盘状BLR的参数变化引起的，首先是内（外）半径的变化，这可以很好地解释周期I谱线参数的变化。谱线轮廓上的巴耳末衰减量呈钟形，不仅受盘内物理过程的影响，还受Ha和Hb谱线的不同发射盘尺寸的影响。3C390.3的BLR的几何形状似乎非常复杂，可能存在流入/流出，但很明显，具有盘状几何形状的宽线区域具有主导发射。
英文摘要：
A study of the variability of the broad emission-line parameters of 3C390.3, an active galaxy with the double-peaked emission-line profiles, is presented. We give a detail analysis of variation in the broad Ha and Hb profiles, the ratios, and the Balmer decrement of different line segments. Studying the variability of the line profiles we explore the disk structure, that is assumed to emit the broad double-peaked Ha and Hb emission lines. We divided the observed spectra in two periods (before and after the outburst in 2002) and analyzed separately the variation in these two periods. First we analyzed the spectral emission-line profiles of Ha and Hb, measuring the peak positions. Then, we divided lines into several segments, and we measured the line-segment fluxes. The Balmer decrement variation for total Ha and Hb fluxes, as well as for the line segments has been investigated and discussed. We modeled the line parameters variation using an accretion disk model. We compared the variability in the observed line parameters with the disk model predictions and found that the variation in line profiles and in line segments corresponds to the emission of a disk-like BLR. But, also there is probably one additional emission component that contributes to the Ha and Hb line center. We found that the variation in the line profiles is caused by the variation in the parameters of the disk-like BLR, first of all in the inner (outer) radius which can well explain the line parameter variations in the Period I. The Balmer decrement across the line profile has a bell-like shape, and it is affected not only by physical processes in the disk, but also by different emitting disk dimension of the Ha and Hb line. The geometry of the BLR of 3C390.3 seems to be very complex, and inflows/outflows might be present, but it is evident that the broad line region with disk-like geometry has dominant emission.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
