论文标题
围绕巨大恒星的风吹星云的电离 - 加速动力模拟
Ionization-Gasdynamic Simulations of Wind-Blown Nebulae around Massive Stars
论文作者
论文摘要
使用采用自洽方法计算光电发对偶尔气体动力学影响的代码，我们对围绕巨大恒星周围的风驱动星云的形成进行建模。我们考虑了恒星特性的变化和恒星演变的质量损失。我们的模拟显示了整个恒星演变的各种属性（例如密度和电离部分）如何变化。多维模拟揭示了在主要序列中存在强电离前端不稳定性的，类似于银河电离锋中所见的阶段。界面处的流体动力学不稳定性导致形成细丝和团块，这些细丝和团块不断被剥离并与低密度内部混合。即使风开始完全径向，球形对称性也很快被破坏，而震惊的风区显然是不对称的。模拟表明，重要的是要包括恒星的光电离光子的效果，而不包括此的光子可能无法重现围绕巨大恒星周围的风吹出气泡的观察到的密度曲线和电离结构。
Using a code that employs a self-consistent method for computing the effects of photo-ionization on circumstellar gas dynamics, we model the formation of wind-driven nebulae around massive stars. We take into account changes in stellar properties and mass-loss over the star's evolution. Our simulations show how various properties, such as the density and ionization fraction, change throughout the evolution of the star. The multi-dimensional simulations reveal the presence of strong ionization front instabilities in the main-sequence phase, similar to those seen in galactic ionization fronts. Hydrodynamic instabilities at the interfaces lead to the formation of filaments and clumps that are continually being stripped off and mixed with the low density interior. Even though the winds start out as completely radial, the spherical symmetry is quickly destroyed, and the shocked wind region is manifestly asymmetrical. The simulations demonstrate that it is important to include the effects of the photoionizing photons from the star, and simulations that do not include this may fail to reproduce the observed density profile and ionization structure of wind-blown bubbles around massive stars.
