Effects of Rotation on the Spatial Structure of Wolf-Rayet Winds

小行星9417186 沃尔夫-拉叶（WR）星的风具有非常大的质量损失率和快速的终端速度。合成的风动量通量大大超过出射辐射场中的风动量通量。 与O型星的风相比，WR风的加速速度似乎相当缓慢，因此适度的恒星旋转可以导致恒星赤道区域密度的显着增强。 本研究旨在发展风的二维模式，并利用“风压缩区”模式来探讨WR星的观测结果。 它基于“风压缩盘”模型，该模型是为快速旋转的Be星开发的。 对于以10%到20%的临界转速旋转的恒星，风压缩可以解释WR星的许多令人困惑的观测性质，例如为什么只有一些WR星显示偏振，以及为什么有紧凑伴星的WR星可以有强烈的X射线发射。 此外，我们将使用我们的2-D WCZ模型来研究亮蓝变星（LBV）。 这些物体被认为是WR阶段的先驱阶段。 LBV被观察到有缓慢的风，有些似乎有轴对称结构（如船底座AG），这表明这些恒星也是我们的旋转风模型的应用程序的良好候选人。 也有证据表明WR星的非热无线电发射，风可能是高能粒子产生的来源。 由于这些观测结果，磁场也将包括在WCZ图片中。 这将使我们能够重新解释观测证据，也使我们能够调查风动力学场的后果。 ***

Cassineli 9417186 Wolf-Rayet (WR) stars have winds with very large mass-loss rates and fast terminal speeds. The resultant wind momentum flux greatly exceeds that in the emergent radiation field. In contrast with the winds of O stars, the WR winds appear to accelerate rather slowly so that moderate stellar rotation can lead to a significant enhancement of the density in the equatorial region of the stars. This research is to develop two-dimensional models of the winds and to investigate the consequences of the structure for the observations of WR stars using the "Wind Compression Zone" model. It is based on the "Wind Compression Disk" model, which was developed for rapidly rotating Be stars. For stars rotating at about 10% to 20% critical, the wind compression may explain a number of puzzling observational properties of WR stars, such as why only some WR stars show polarization and why WR stars with compact companions can have strong X-ray emission. In addition, we will study the Luminous Blue Variables (LBVs) using our 2-D WCZ model. These objects are thought to be a precursor stage to the WR phase. LBVs are observed to have slow winds, and some appear to have axisymmetric structure (e.g. AG Carinae), which indicates that these stars are also good candidates for the application of our rotating wind model. There is also evidence of non-thermal radio emission from WR stars and that the winds might be source of high energy particle production. Because of these observations magnetic fields will also be included in the WCZ picture. This will allow us to re-interpret the observational evidence, and also allow us to investigate the consequences of the fields on the wind dynamics. ***