Radiation Hydrodynamic Simulations of Dust-driven Winds
Radiation Hydrodynamic Simulations of Dust-driven Winds
复制标题
尘埃驱动风的辐射流体动力学模拟
DOI：
10.3847/1538-4357/aa6935
复制
发表时间：
2016
期刊：
影响因子：
--
通讯作者：
S. Davis
中科院分区：
文献类型：
--
作者：
Dong Zhang;S. Davis
我们研究由快速恒星形成环境中大气辐射压力驱动的尘埃风。我们应用可变Eddington张量算法重新研究了在恒定红外辐射通量下加速的气体柱的二维辐射流体动力学问题。在没有重力的情况下，系统的主要特征是气体的初始光学深度。我们用不同的初始光学深度和分辨率进行了几次运行。我们发现，随着平均速度和速度弥散的增加，气体沿垂直方向扩散。与先前使用通量限制扩散算法的工作相比，我们发现捕获因子的变化很小。在没有重力的情况下，辐射和气体之间的动量耦合与有重力的情况类似。对于Eddington比随系统高度的增加，辐射向气体的动量传递不仅被放大，而且被放大了一个因子，其中为通过系统的红外积分光学深度，随着光学深度的增加而减小。我们将我们的结果应用于星系的大气，并得出结论，辐射压力可能是在最快速形成恒星的星系和星暴中驱动风的重要机制。
We study dusty winds driven by radiation pressure in the atmosphere of a rapidly star-forming environment. We apply the variable Eddington tensor algorithm to re-examine the two-dimensional radiation hydrodynamic problem of a column of gas that is accelerated by a constant infrared radiation flux. In the absence of gravity, the system is primarily characterized by the initial optical depth of the gas. We perform several runs with different initial optical depths and resolutions. We find that the gas spreads out along the vertical direction, as its mean velocity and velocity dispersion increase. In contrast to previous work using the flux-limited diffusion algorithm, we find little evolution in the trapping factor. The momentum coupling between radiation and gas in the absence of gravity is similar to that with gravity. For Eddington ratio increasing with the height in the system, the momentum transfer from the radiation to the gas is not merely , but amplified by a factor of , where is the integrated infrared optical depth through the system, and , decreasing with the optical depth. We apply our results to the atmosphere of galaxies and conclude that radiation pressure may be an important mechanism for driving winds in the most rapidly star-forming galaxies and starbursts.