论文标题
3c 390.3核的光谱变异性超过20年 - ii。广泛的排放线轮廓的可变性和ii $ \ lambda4686 $ a发射线通量
Spectral variability of the 3C 390.3 nucleus for more than 20 years -- II. Variability of the broad emission-line profiles and He II $\lambda4686$A emission-line fluxes
论文作者
论文摘要
H $β$和H $α$宽发射线轮廓以及He II $ \ lambda4686 $的变异性的分析结果存在于1992-2014期间的3C 390.3核中的发射线通量。尽管存在一些差异，但观察到的Balmer线的速度依赖性滞后与开普勒盘构型的预期相似。除了开普勒旋转外，可能存在径向插入运动的3C 390.3区域。 Broad He II线的滞后是$ 26 \ pm 8 $ D，大大低于Balmer线的差，因此He II排放区域的尺寸要小得多。就线条和光学连续通量之间的幂律关系而言，逐渐变化的比例尺factor $ c（t）$：$ f_ {line} \ propto c（t）\，f_ {cont}^a $，power $ a $ a $ a $ a $ a $ a $ a $ a $ a $ a $ as in Broad He ii line line in ii ii doper power for power for power for $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $。线分别。这意味着可变性幅度是HE II中最大的，在H $β$中较少，而在H $α$中更少。但是，Balmer线包含长期趋势，在氦气线上看不到。狭窄的HE II线是可变的，幅度（最大值比率）$ r_ {max} \大约3 $，远高于窄级Balmer线和窄[O III] $λ$ 5007A线的可变性幅度。
Results of the analysis of the variability of the H$β$ and H$α$ broad emission-line profiles and the He II $\lambda4686$A emission-line fluxes in the 3C 390.3 nucleus during 1992-2014 are present. The observed velocity-dependent lag for the Balmer lines is similar to that expected from the Keplerian disc configuration, although there are some differences. Probably, a radial infall motion can be present in the broad-line region of 3C 390.3 in addition to the Keplerian rotation. The lag of the broad He II line is $26\pm 8$d, significantly less than that of the Balmer lines, so the He II emission region is much smaller in size. In terms of the power-law relationship between line and optical continuum fluxes with slowly varying scalefactor $c(t)$: $F_{line}\propto c(t)\,F_{cont}^a$, the power $a$ is $1.03$ for the broad He II line, while according to Paper I the power is equal to $0.77$ and $0.54$ for the broad H$β$ and H$α$ lines, respectively. It means that the variability amplitude is the largest in the He II, less in H$β$, and more less in H$α$. However, the Balmer lines contain a long-term trend that is not seen in the helium line. The narrow He II line is variable with the amplitude (max-to-min ratio) $R_{max}\approx 3$ that is much greater than the variability amplitudes of both the narrow Balmer lines and the narrow [O III] $λ$5007A line.
