宽吸收线类星体的极地+赤道风模型：I。拟合C IV BAL轮廓
A polar+equatorial wind model for broad absorption line quasars: I. Fitting the C IV BAL profiles
摘要：
尽管所有的研究，在近20%的类星体中观察到的蓝移宽吸收线（BAL）起源处的风的几何形状仍然是一个争论的问题。我们想看看一个两个组成部分的极地+赤道风的几何形状可以重现在这些对象中观察到的典型的BAL配置文件。我们建立了一个Monte Carlo辐射转移代码（称为MCRT）来模拟在极+赤道风中形成的线轮廓，其中从球对称核发射的光子被共振散射。我们的目标是再现典型的C IV线轮廓观察到的BAL类星体，并确定参数的线轮廓。双分量风模型似乎是有效的复制BAL配置文件从P Cygni型配置文件更复杂的。某些剖面也可以通过杆上视图进行复制。我们的模拟提供的证据表明，在BAL类星体与非P天鹅型线配置文件的极轴周围的风的高速旋转。
英文摘要：
Despite all the studies, the geometry of the wind at the origin of the blueshifted broad absorption lines (BAL) observed in nearly 20% of quasars still remains a matter of debate. We want to see if a two-component polar+equatorial wind geometry can reproduce the typical BAL profiles observed in these objects. We built a Monte Carlo radiative transfer code (called MCRT) to simulate the line profiles formed in a polar+equatorial wind in which the photons, emitted from a spherically symmetric core are resonantly scattered. Our goal is to reproduce typical C IV line profiles observed in BAL quasars and to identify the parameters governing the line profiles. The two-component wind model appears to be efficient in reproducing the BAL profiles from the P Cygni-type profiles to the more complex ones. Some profiles can also be reproduced with a pole-on view. Our simulations provide evidence of a high-velocity rotation of the wind around the polar axis in BAL quasars with non P Cygni-type line profiles.
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