论文标题
使用排球网状分解的太阳对流区域的全球MHD模拟。 I.飞行员
Global MHD simulations of the solar convective zone using a volleyball mesh decomposition. I. Pilot
论文作者
论文摘要
由于缺乏连接时上和时间上不同尺度的工具，以及涉及的广泛不同的环境和涉及的物理效果，太阳能建模长期以来一直被分为“内部”和“表面”建模。最近，已经付出了重大努力来解决这一脱节。我们使用基于任务的调度代码框架，将内部对流区和发电机模拟连接到太阳表面的杰出瓶颈，并进行概念验证的高分辨率全球模拟。我们提出了一个新的“排球”网状分解，它的笛卡尔斑块在没有奇异性的球体上被切成薄片。我们使用新的基于熵的HLLS近似Riemann求解器在全球模拟中对磁性流差动力学进行建模，范围在0.655-0.995 r $ _ \ odot $之间，初始环境磁场设置为0.1高斯。模拟通过复杂的湍流结构产生对流运动。小规模的发电机动作扭曲了环境磁场，并在初始运行时内将磁场幅度放大了两个以上的数量级。
Solar modelling has long been split into ''internal'' and ''surface'' modelling, because of the lack of tools to connect the very different scales in space and time, as well as the widely different environments and dominating physical effects involved. Significant efforts have recently been put into resolving this disconnect. We address the outstanding bottlenecks in connecting internal convection zone and dynamo simulations to the surface of the Sun, and conduct a proof-of-concept high resolution global simulation of the convection zone of the Sun, using the task-based DISPATCH code framework. We present a new `volleyball' mesh decomposition, which has Cartesian patches tessellated on a sphere with no singularities. We use our new entropy based HLLS approximate Riemann solver to model magneto-hydrodynamics in a global simulation, ranging between 0.655 -- 0.995 R$_\odot$, with an initial ambient magnetic field set to 0.1 Gauss. The simulations develop convective motions with complex, turbulent structures. Small-scale dynamo action twists the ambient magnetic field and locally amplifies magnetic field magnitudes by more than two orders of magnitude within the initial run-time.
