Hydrodynamical Models of Line-driven Accretion Disk Winds
Hydrodynamical Models of Line-driven Accretion Disk Winds
复制标题
线驱动吸积盘风的流体动力学模型
DOI：
10.1086/303671
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发表时间：
1997
期刊：
影响因子：
--
通讯作者：
J. Blondin
中科院分区：
文献类型：
--
作者：
Nicolas A. Pereyra;T. Kallman;J. Blondin
本文给出了来自激变系统的线驱动吸积盘风的一维解析水动力模型以及一维和二维数值水动力模型。利用一维解析模型，我们探讨了圆盘风存在的物理条件，并研究了风速和质量损失率与半径的关系。我们的二维模型的结果与从极地风性质的CVs观测到的光谱、在P天鹅座廓线末端速度的大约一半处的最大吸收以及末端速度的数量级是一致的。对于视盘光度LDISK=L☉，白矮星质量MWD=0.6M☉，视盘半径RDISK=R☉，声速a=10 KM S-1，得到风质量损失率ṀWind=2×10−14Myr-1，终端风速约3000 KM S-1。二维模型表明，离心力在圆盘风中产生激波。如果没有这些激波，得到的质量损失率将太低，无法产生解释P天鹅座星云轮廓所需的光学深度。二维模型证明了来自吸积盘的风中离心力的重要性，从而证明了可以表示这些力的模型的必要性。
We present here one-dimensional analytic hydrodynamic models and both one-dimensional and two-dimensional numerical hydrodynamic models for line-driven accretion disk winds from cataclysmic variable (CV) systems. Using the one-dimensional analytic models we explore the physical conditions necessary for the existence of a disk wind and study the dependence of wind speed and mass-loss rate on radius. The results of our two-dimensional model are consistent with the spectrum observed from CVs in the polar nature of the wind, the maximum absorption at roughly half the terminal speed of the P Cygni profiles, and the order of magnitude of the terminal speeds. For disk luminosity Ldisk = L☉, white dwarf mass Mwd = 0.6 M☉, disk radius Rdisk = R☉, and sound speed a = 10 km s-1 we obtain a wind mass-loss rate of Ṁwind=2 × 10−14 M yr-1 and a terminal velocity of ~3000 km s-1. The two-dimensional models show that centrifugal forces produce shocks in the disk wind. If these shocks were absent, the mass-loss rates obtained would be too low to produce the optical depths required to explain the P Cygni profile of CVs. The two-dimensional models demonstrate the importance of centrifugal forces in winds from accretion disks and thus the necessity of models where these forces may be represented.