Eclipse Mapping of the Accretion Disk Wind in the Cataclysmic Variable UX Ursae Majoris
Eclipse Mapping of the Accretion Disk Wind in the Cataclysmic Variable UX Ursae Majoris
复制标题
大熊座灾难变星 UX 中吸积盘风的日食映射
DOI：
10.1086/304519
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发表时间：
1997
期刊：
影响因子：
--
通讯作者：
J. Drew
中科院分区：
文献类型：
--
作者：
C. Knigge;J. Drew
我们提出了一个努力的结果，以模拟最近的HST日食观测的C IV 1550年的共振线在高倾角新星般的激变变量UX UMa。假设这条线主要是风形成的，我们能够大致再现的形状和强度的观测线轮廓（远离和在日食期间）的一个简单的运动学模型的框架内，外流被描述为一个旋转的，双锥吸积盘风。我们的首选模型也匹配的大部分的详细行为的不同部分的C IV线轮廓（蓝翼，线中心，和红翼）作为轨道相位的函数。我们的模拟结果最重要的是，它强烈地暗示了在盘光球和快速移动的风之间存在一个高柱（NH ~ 1023 cm-2），相对密集（Ne = 4 × 1012 cm-3），并且只有缓慢流出（vpoloidal vescape）的过渡区。我们还发现，来自UX UMa的流出可能只是适度准直（我们首选模型的外开角为θmax <$65 °）。最后，我们的模型相当好地拟合了数据中看到的旋转扰动，其中风中运动的旋转分量通过保持流出物质的特定角动量而固定。这些结果的影响，磁盘驱动风的动力学模型进行了讨论。
We present the results of an effort to model recent HST eclipse observations of the C IV 1550 Å resonance line in the high-inclination nova-like cataclysmic variable UX UMa. Assuming this line to be predominantly wind-formed, we are able to roughly reproduce the shapes and strengths of the observed line profiles (both away from and during eclipse) within the framework of a simple kinematic model in which the outflow is described as a rotating, biconical accretion disk wind. Our preferred model also matches most of the detailed behavior of different parts of the C IV line profile (blue wing, line center, and red wing) as a function of orbital phase. The most important result of our modeling is that it strongly suggests the presence of a high column (NH ~ 1023 cm-2), relatively dense (ne ≃ 4 × 1012 cm-3), and only slowly outflowing (vpoloidal ≪ vescape) transition region between the disk photosphere and the fast-moving wind. We also find that the outflow from UX UMa is probably only moderately collimated (the outer opening angle of our preferred model is θmax ≃ 65°). Finally, the rotational disturbance seen in the data is fitted reasonably well by our model, in which the rotational component of motion in the wind is fixed by conserving the specific angular momentum of the outflowing material. The implications of these results for dynamical models of disk-driven winds are discussed.