谱线移动、宽线区流入和活动星系核的馈送
Line Shifts, Broad-Line Region Inflow, and the Feeding of AGNs
摘要：
速度分辨混响映射表明，宽线区域（BLR）的活动星系核可以有显着的净流入。我们使用的斯托克斯辐射转移代码显示，电子和瑞利散射关闭的BLR和环面自然解释了高电离线的蓝移的档案和蓝移的电离依赖性。该结果对散射区域的几何形状不敏感。如果正确的话，这个模型解决了速度分辨混响映射所隐含的外流的缺乏和如果蓝移是遮蔽的结果则需要外流之间的长期冲突。由流入所暗示的吸积速率足以为活动星系核提供动力。我们认为BLR是外吸积盘的一部分，并且类似的MHD过程正在运行。在散射模型中，蓝移与吸积率成正比，因此高吸积率活动星系核将表现出更大的高电离线蓝移。散射会导致从C IV线得到的系统性过高的黑洞质量估计。我们注意到窄线区（NLR）和BLR蓝移之间的许多相似之处，并建议NLR蓝移有一个类似的解释。我们的模型解释了更高的蓝移宽吸收线类星体，如果他们更高度倾斜。对于活动星系核周围的中性物质，来自BLR和环面的瑞利散射可能比电子散射更重要。瑞利散射与电子散射的重要性可以通过比较来自同一发射线区域的不同波长的线轮廓来评估。
英文摘要：
Velocity-resolved reverberation mapping suggests that the broad-line regions (BLRs) of AGNs can have significant net inflow. We use the STOKES radiative transfer code to show that electron and Rayleigh scattering off the BLR and torus naturally explains the blueshifted profiles of high-ionization lines and the ionization dependence of the blueshifts. This result is insensitive to the geometry of the scattering region. If correct, this model resolves the long-standing conflict between the absence of outflow implied by velocity-resolved reverberation mapping and the need for outflow if the blueshifting is the result of obscuration. The accretion rate implied by the inflow is sufficient to power the AGN. We suggest that the BLR is part of the outer accretion disk and that similar MHD processes are operating. In the scattering model the blueshifting is proportional to the accretion rate so high-accretion-rate AGNs will show greater high-ionization line blueshifts as is observed. Scattering can lead to systematically too high black hole mass estimates from the C IV line. We note many similarities between narrow-line region (NLR) and BLR blueshiftings, and suggest that NLR blueshiftings have a similar explanation. Our model explains the higher blueshifts of broad absorption line QSOs if they are more highly inclined. Rayleigh scattering from the BLR and torus could be more important in the UV than electron scattering for predominantly neutral material around AGNs. The importance of Rayleigh scattering versus electron scattering can be assessed by comparing line profiles at different wavelengths arising from the same emission-line region.
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