论文标题
J132216.25+052446.3中多相超快速流出的协调时间变化
Coordinated time variability of multi-phase ultra-fast outflows in J132216.25+052446.3
论文作者
论文摘要
我们介绍了在J132216.25+052446.3（z（em）= 2.04806）的频谱中看到的宽吸收线（BAL;分布在5800-29000 km/s）的宽度吸收线的时间变化分析。最强的吸收成分（BAL-A；分布在5800-9900 km/s上）由几个狭窄的组件组成，其速度分离接近C IV Doublet分裂。 BAL-A的C IV，N V和SI IV吸收显示相关的光学深度变异性，而速度结构没有显着变化。在我们的监测期间，出现了非常宽且浅的吸收（BAL-C；分布在速度范围15000-29000 km/s上），与J1322+0524的调度发作相吻合。所有确定的吸收线均显示与随着磁通量减少的等效宽度的相关性变异性。这与C IV发射线变异性一致，与电离是相关变异性的主要驱动力。观察到的紫外线变化比光电报模型所要求的要弱。如果C IV电离光子的变化远大于UV连续体的变化，则可以理解在给定连续通量处的C IV等效宽度中的散射，而电离光子和UV通量的变化与流动覆盖率不相关，并且流动覆盖率不断变化。我们建议BAL-A是由位于宽发射线区域以外的稳定块状流出产生的，而BAL-C是位于积聚盘附近的新形成的风组分，并且都对电离连续体的变化做出了反应。
We present a time variability analysis of broad absorption lines (BAL; spread over the velocity range of 5800-29000 km/s) seen in the spectrum of J132216.25+052446.3 (z(em)= 2.04806) at ten different epochs spanning over 19 years. The strongest absorption component (BAL-A; spread over 5800-9900 km/s) is made up of several narrow components having velocity separations close to C IV doublet splitting. The C IV, N V, and Si IV absorption from BAL-A show correlated optical depth variability without significant changes in the velocity structure. A very broad and shallow absorption (BAL-C; spread over the velocity range 15000-29000 km/s) emerged during our monitoring period coinciding with a dimming episode of J1322+0524. All the identified absorption lines show correlated variability with the equivalent widths increasing with decreasing flux. This together with the C IV emission-line variability is consistent with ionization being the main driver of the correlated variability. The observed UV-continuum variations are weaker than what is required by the photo-ionization models. This together with a scatter in the C iv equivalent width at a given continuum flux can be understood if variations of the C IV ionizing photons are much larger than that of the UV continuum, the variations in the ionizing photon and UV fluxes are not correlated and/or the covering factor of the flow varies continuously. We suggest BAL-A is produced by a stable clumpy outflow located beyond the broad emission line region and BAL-C is a newly formed wind component located near the accretion disk and both respond to changes in the ionizing continuum.
