论文标题
中间质量恒星中的内重力波诱导的化学混合
Chemical Mixing Induced by Internal Gravity Waves in Intermediate Mass Stars
论文作者
论文摘要
内部重力波（IGW）会导致恒星的辐射内部混合。我们通过将示踪剂颗粒引入两个维度（2D）流体动力学模拟来研究这种混合。在Rogers＆McElwaine（2017），Arxiv：1709.04920之后，我们将研究扩展到不同的群众（3 m $ _ {\ odot} $，7 m $ _ {\ odot} $和20 m $ _ $ _ {\ odot} $）和ZAMS，MIDMS和MIDMS和TAMS）。这些模型的扩散曲线受到各种参数的影响，例如Brunt-Väisälälälälälälälälälälälälä，密度，热阻尼，几何效应以及有助于这些混合曲线的波的频率。我们发现混合曲线在各个年龄段都发生了巨大变化。在年轻的恒星中，我们注意到扩散系数向表面升高，而在较老的恒星中，扩散曲线的初始增加之后是趋势下降。我们还发现，在更大的恒星中混合更强。因此，未来的恒星进化模型应包括此变化。为了帮助将这种混合包含在一维（1D）恒星演化模型中，我们确定了有助于这些混合曲线的主要波，并提出可以包含在1D模型中的处方。
Internal gravity waves (IGWs) can cause mixing in the radiative interiors of stars. We study this mixing by introducing tracer particles into two - dimensional (2D) hydrodynamic simulations. Following the work of Rogers & McElwaine (2017), arXiv:1709.04920, we extend our study to different masses (3 M$_{\odot}$, 7 M$_{\odot}$ and 20 M$_{\odot}$) and ages (ZAMS, midMS and TAMS). The diffusion profiles of these models are influenced by various parameters such as the Brunt-Väisälä frequency, density, thermal damping, the geometric effect and the frequencies of waves contributing to these mixing profiles. We find that the mixing profile changes dramatically across age. In younger stars, we noted that the diffusion coefficient increases towards the surface, whereas in older stars the initial increase in the diffusion profile is followed by a decreasing trend. We also find that mixing is stronger in more massive stars. Hence, future stellar evolution models should include this variation. In order to aid the inclusion of this mixing in one-dimensional (1D) stellar evolution models, we determine the dominant waves contributing to these mixing profiles and present a prescription that can be included in 1D models.
