论文标题
磁性恒星气泡的仿真
Simulations of Magnetised Stellar-Wind Bubbles
论文作者
论文摘要
最初的结果来自O恒星周围的恒星气泡的3D MHD建模，通过ISM副人移动。我们描述了以合理的计算成本启用高分辨率3D MHD模拟的算法更新。我们将方法应用于旋转巨大恒星的天气圈的模拟，以30 km/s通过漫射的星际介质移动，以描述了两种不同的恒星磁场强度，10 g和100 g。流动中的特征并与地层的类似模型进行了比较。震惊的星际介质随着恒星的运动方向未对准的磁场而变得不对称，并有可观察的后果。当风的马赫数为$ \ leq $ 10时，恒星磁场开始影响风气泡的结构，并且与恒星的磁轴相关的特征在parsec尺度上可见。讨论了预测和测量非热辐射的前景。
Initial results are presented from 3D MHD modelling of stellar-wind bubbles around O stars moving supersonically through the ISM. We describe algorithm updates that enable high-resolution 3D MHD simulations at reasonable computational cost. We apply the methods to the simulation of the astrosphere of a rotating massive star moving with 30 km/s through the diffuse interstellar medium, for two different stellar magnetic field strengths, 10 G and 100 G. Features in the flow are described and compared with similar models for the Heliosphere. The shocked interstellar medium becomes asymmetric with the inclusion of a magnetic field misaligned with the star's direction of motion, with observable consequences. When the Alfvenic Mach number of the wind is $\leq$10 then the stellar magnetic field begins to affect the structure of the wind bubble and features related to the magnetic axis of the star become visible at parsec scales. Prospects for predicting and measuring non-thermal radiation are discussed.
