论文标题
解释AGB星星的风：最近的进步
Explaining the winds of AGB stars: Recent progress
论文作者
论文摘要
在渐近巨型分支（AGB）恒星周围观察到的风通常归因于灰尘上的辐射压力，这是在这些脉动，强烈对流恒星的扩展动力大气中形成的。当前的辐射流动力学模型可以解释许多观察到的特征，它们正处于提供质量损失的预测理论的边缘。这篇综述总结了最新的结果和对AGB恒星风的持续工作，讨论了驾驶机制的关键成分，以及全球3D RHD恒星和磁盘模拟的第一个结果。通过这样的模型，有可能在整个3D几何形状中遵循物质流，从AGB恒星的湍流，脉动内部，通过其大气和灰尘形成区域到尘埃辐射压力加速风的区域。可以解决风的恒星气氛的高级仪器为测试模型提供了必不可少的数据。
The winds observed around asymptotic giant branch (AGB) stars are generally attributed to radiation pressure on dust, which is formed in the extended dynamical atmospheres of these pulsating, strongly convective stars. Current radiation-hydrodynamical models can explain many of the observed features, and they are on the brink of delivering a predictive theory of mass loss. This review summarizes recent results and ongoing work on winds of AGB stars, discussing critical ingredients of the driving mechanism, and first results of global 3D RHD star-and-wind-in-a-box simulations. With such models it becomes possible to follow the flow of matter, in full 3D geometry, all the way from the turbulent, pulsating interior of an AGB star, through its atmosphere and dust formation zone into the region where the wind is accelerated by radiation pressure on dust. Advanced instruments, which can resolve the stellar atmospheres, where the winds originate, provide essential data for testing the models.
