Collaborative Research: SHINE: Driving Solar Magnetohydrodynamic (MHD) Simulations with Vector Magnetogram Sequences

这些pi建议合作开发新技术，以测量太阳大气的状态，并解决控制其演变的物理方程。提议者计划将这些能力结合起来，这样数值模拟就可以直接由观测到的太阳数据驱动。为了实现这一目标，他们打算开发新的方法来减少太阳矢量磁图序列，优化输入到模拟中，作为数值解的自一致的边界条件集。将使用半隐式代码来求解受这些初始条件和边界条件约束的可压缩时变磁流体动力学（MHD）方程。这些新方法提供的端到端能力将通过对至少三个太阳活动区进行数据驱动模拟来证明。几十年来，通过地面和太空仪器的高质量观测，研究人员提出了几种不同的日冕物质抛射的起源和演化模型。三维的、时间相关的模拟可以证明这些模型的可行性，只要它们得到适当的驱动。然而，只有直接用数据驱动这些模拟才能确定最能描述现实的模型。这项建议将发展进行这种试验的必要技术，并将有助于发展国家空间天气预报能力，这种能力将把正在进行的观测结果纳入求解控制方程的大规模计算机模拟。在这项工作下开发的所有工具都将向太阳物理界和公众开放。

The PIs propose to collaborate in developing new techniques for measuring the state of the solar atmosphere and for solving the physical equations governing its evolution. The proposers plan to combine these capabilities so that numerical simulations might be directly driven by observed solar data. To accomplish this, they intend to develop new methods of reducing solar vector magnetogram sequences, optimized for input into simulations as a self-consistent set of boundary conditions for a numerical solution. A semi-implicit code will be used to solve the compressible, time-dependent magnetohydrodynamic (MHD) equations subject to those initial conditions and boundary conditions. The end-to-end capability provided by these new methods will be demonstrated by performing data-driven simulations of at least three solar active regions. Decades of high-quality observations from ground-based and space-based instruments have led researchers to propose several different models for the origin and evolution of coronal mass ejections. Three-dimensional, time-dependent simulations can demonstrate the viability of these models, provided they are appropriately driven. However, only driving these simulations directly with data can identify the model that best describes reality. This proposal will develop the necessary techniques to perform such a test, and will contribute to the development of a national space weather forecasting capability, which will assimilate ongoing observations into large-scale computer simulations that solve the governing equations. All tools developed under this effort will be made available to the solar physics community and to the public.