SHINE: Using Magnetohydrodynamic (MHD) Simulations to Test Methods of Measuring Photospheric Velocities

数值模拟预测日冕物质抛射（CME）需要太阳光球层等离子体的实际速度场的规范。 这些信息必须从代用磁图观测中“导出”，这可能导致推断流场的错误和不准确。 将采用太阳磁对流的现实数值模拟来模拟合成磁图。 然后使用SHINE社区中的观察者提供的方案，通过（i）局部相关跟踪，（ii）特征跟踪和（iii）最小能量拟合技术来“导出”速度场。 通过将这些推断的速度场与已知的流进行比较，可以（i）确定哪些方法最准确地确定速度，（ii）表征方法中的病理，（iii）建议补救这些病理的方法，以及（iv）将这些结果传播给太阳物理学/SHINE社区中这些方法的许多用户。

Numerical simulations aimed at forecasting solar Coronal Mass Ejections (CMEs) require specification of the actual velocity field of the plasma at the solar photosphere. This information must be "derived" from proxy magnetogram observations, and this can lead to errors and inaccuracies in the inferred flow fields. Realistic numerical simulations of solar magnetoconvection will be employed to simulate synthetic magnetograms. Then using schemes provided by observers in the SHINE community the velocity field will be "derived" through, (i) local-correlation tracking, (ii) feature tracking, and (iii) minimum energy fitting techniques. By comparing these inferred velocity fields against the known flows one may, (i) identify which methods most accurately determine velocities, (ii) characterize pathologies in the methods, (iii) suggest ways to remedy these pathologies, and (iv) disseminate these results to the many users of these methods in the solar physics/SHINE communities.