Radiation driven winds from hot stars: hydrodynamic models with detailed non-LTE radiative transfer

比太阳大得多的恒星在宇宙演化中起着重要作用。作为它们的特殊属性，它们拥有恒星风，可以将大量物质吹到它们的环境中。必须首先考虑辐射压力作为驱动机制。虽然这对部分恒星来说是相当好的理解，但模型只适用于那些最强的恒星风，即所谓的沃尔夫-拉叶星。经过初步研究，我们可以假设这些强风也可以用辐射压力来解释。如果是这样，以前的水动力学模型的相应不足一定是由于它们在处理辐射转移时的某些近似。波茨坦沃尔夫-拉叶（PoWR）模式大气代码避免了这种简化，我们已经开发了光谱的模拟和分析。正如我们已经表明的那样，这个代码可以与流体动力学方程结合起来。在建议的项目中，我们将把这些模型计算发展成一种可以常规应用的形式。然后，与观测结果的比较将揭示密集的恒星风是否可以用辐射压力来解释。最终目标是现实的模型预测，这对于理解大质量恒星的演化和物质的宇宙循环是必需的。

Stars much more massive than the sun play an important role in the cosmic evolution. As their special property, they possess stellar winds that blow lots of matter into their environment. Radiation pressure must be considered in the first place as the driving mechanism. While this is reasonably well understood for part of the stars, the models fail just for the strongest of those stellar winds, which emerge from the so-called Wolf-Rayet stars. After pilot studies we can assume that those strong winds can also be explained by radiation pressure. If so, the corresponding shortfall of previous hydrodynamical models must be due to certain approximations in their treatment of radiative transfer.Such simplifications are avoided by the Potsdam Wolf-Rayet (PoWR) model atmosphere code, which we have developed for the simulation and analysis of spectra. As we have already shown, this code can be combined with the hydrodynamic equations. In the proposed project we will develop these model calculation into a form that they can be routinely applied. Then the comparison with observations will reveal if the dense stellar winds can be generally explained by radiation pressure. The final goal are realistic model predictions, which are needed for understanding the evolution of massive stars and the cosmic circuit of matter.