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

用于预测日冕物质抛射(CME)的数值模拟需要描述太阳光球处等离子体的实际速度场。这些信息必须来自代理磁图观测，这可能会在推断的流场中导致错误和不准确。太阳磁对流的真实数值模拟将被用来模拟合成磁图。然后，使用SISH社区中的观察者提供的方案，将通过(I)局部相关跟踪、(Ii)特征跟踪和(Iii)最小能量拟合技术来“推导”速度场。通过将这些推断的速度场与已知的流动相比较，可以(I)确定哪些方法最准确地确定速度，(Ii)表征这些方法中的病态，(Iii)提出补救这些病态的方法，以及(Iv)将这些结果传播给太阳物理/阳光社区中使用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.