Modeling the Spectral Signatures of Accretion Disk Winds: A New Monte Carlo Approach
Modeling the Spectral Signatures of Accretion Disk Winds: A New Monte Carlo Approach
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吸积盘风的频谱特征建模：一种新的蒙特卡罗方法
DOI：
10.1086/342879
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发表时间：
2002
期刊：
影响因子：
--
通讯作者：
C. Knigge
中科院分区：
文献类型：
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作者：
K. Long;C. Knigge
双极外流存在于许多盘吸积天体物理系统中。在盘吸积激变变星(CV)中，这些外流是这些系统紫外线光谱中大部分强烈特征的原因。然而，很少有人尝试对这些特征进行定量建模。在这里，我们描述了一种新的、混合的蒙特卡罗/索博列夫代码，它允许我们合成一个以磁盘为主的、质量损失的CV的完整光谱。我们为C IV计算的线条轮廓类似于以前的工作人员在假设相同的几何形状时计算的线条轮廓。然而，我们的合成光谱不仅显示了众所周知的O VI、N V、Si IV和C IV的共振线，而且在适当选择质量损失率和风的几何形状的情况下，还显示了许多来自激发低态的谱线。在霍普金斯紫外线望远镜、远紫外光谱探测器和哈勃太空望远镜获得的CVS的远紫外线光谱中，已经看到了许多这样的谱线。为了说明我们目前能够再现观测光谱的程度，我们最后给出了一个对爆发中的矮新星Z凸轮的霍普金斯紫外望远镜光谱的初步拟合。
Bipolar outflows are present in many disk-accreting astrophysical systems. In disk-accreting cataclysmic variables (CVs), these outflows are responsible for most of the strong features in the ultraviolet spectra of these systems. However, there have been few attempts to model these features quantitatively. Here we describe a new, hybrid Monte Carlo/Sobolev code, which allows us to synthesize the complete spectrum of a disk-dominated, mass-losing CV. The line profiles that we calculate for C IV resemble those calculated by previous workers when an identical geometry is assumed. However, our synthetic spectra exhibit not only the well-known resonance lines of O VI, N V, Si IV, and C IV but, with an appropriate choice of mass-loss rate and wind geometry, also many lines originating from excited lower states. Many of these lines have already been seen in the far-ultraviolet spectra of CVs obtained with the Hopkins Ultraviolet Telescope, the Far Ultraviolet Spectroscopic Explorer, and the Hubble Space Telescope. In order to illustrate the degree to which we are currently able to reproduce observed spectra, we finally present a preliminary fit to the Hopkins Ultraviolet Telescope spectrum of the dwarf nova Z Cam in outburst.