论文标题
模拟快速旋转星的外层
Simulating the outer layers of rapidly rotating stars
论文作者
论文摘要
本文介绍了一组快速旋转恒星近表面区域中对流的辐射流体动力（RHD）模拟的结果。模拟使用与恒星模型一致的微物理学，并包括逼真的对流和辐射转移的效果。我们发现旋转的总体效果是降低湍流的强度。旋转和辐射冷却的组合产生了区域速度曲线，其中表面附近的流体包裹的运动与旋转无关。它们的运动受辐射冷却产生的强上下流的控制。另一方面，较深层中的流体包裹是通过旋转控制的。
This paper presents the results of a set of radiative hydrodynamic (RHD) simulations of convection in the near-surface regions of a rapidly rotating star. The simulations use microphysics consistent with stellar models, and include the effects of realistic convection and radiative transfer. We find that the overall effect of rotation is to reduce the strength of turbulence. The combination of rotation and radiative cooling creates a zonal velocity profile in which the motion of fluid parcels near the surface is independent of rotation. Their motion is controlled by the strong up and down flows generated by radiative cooling. The fluid parcels in the deeper layers, on the other hand, are controlled by rotation.
