标题： 活动星系核恒星风的线发射 显示英文标题

标题： Line Emission from Stellar Winds in Active Galactic Nuclei

摘要： 本文介绍了活动星系核红巨星恒星线发射模型的合成光谱和响应函数。 我们的结果在模型不确定性范围内与活动星系核的基本线发射特征一致，前提是以下附加假设成立：1）平均恒星质量损失率随远离黑洞的距离而减小；2）平均电离参数低于Kazanas（1989）所提出的值。 对于质量损失增强的模型，线轮廓的零强度全宽与黑洞质量呈1/3次方的比例关系。 这一比例关系表明NLS1s（窄线赛弗特1型星系）的黑洞质量相对较低。 质量损失增强的模型还预测了最小的线/连续延迟与线轮廓的零强度全宽成正比。 由于这些模型具有较高的柱密度，它们产生了三角形形状的响应函数，这在观测中并不常见。 另一方面，没有增强质量损失的模型预测了线-连续延迟与连续光度的平方根成正比，这与经验结果一致。 具有足够高的云间（星际）介质密度以及BLR遮挡吸积盘的模型具有线位移。 类似于C IV、N V和O VI的线的最宽发射和吸收轮廓分量呈现红移。 相反，在这类模型中，最窄的发射和吸收轮廓分量呈现蓝移。 这些结果似乎与观测结果相符（例如，Done & Krolik 1996）。 显示英文摘要

摘要： This dissertation presents synthetic spectra and response functions of the red giant stellar line emission model of active galactic nuclei. Our results agree with the fundamental line emission characteristics of active galactic nuclei within the model uncertainties if the following additional assumptions are made: 1) the mean stellar mass loss rates decrease with distance from the black hole, and 2) the mean ionization parameters are lower than those postulated in Kazanas (1989). For models with enhanced mass loss, the zero-intensity-full-widths of the line profiles are proportional to the black hole mass to the power of 1/3. This scaling relation suggests that the black hole masses of NLS1s (narrow-line Seyfert 1s) are relatively low. Models with enhanced mass loss also predict minimum line/continuum delays that are proportional to the zero-intensity-full-widths of the profiles. Because of their high column densities, these models yield triangle-shaped response functions, which are not generally observed. On the other hand, models without enhanced mass loss yield line-continuum delays that are proportional to the square root of the continuum luminosity, which is constant with empirical results. Models with high enough intercloud (interstellar) medium densities and a BLR-occulting accretion disk have line shifts. The broadest line emission and absorption profile components of lines similar to C IV, N V, and O VI are redshifted. Conversely, the narrowest emission and absorption profile components are blueshifted in such models. These results appear to agree with observations (e.g., Done & Krolik 1996).