The Coronal Global Evolutionary Model (CGEM) provides data-driven simulations of the magnetic field in the solar corona to better understand the build-up of magnetic energy that leads to eruptive events. The CGEM project has developed six capabilities. CGEM modules (1) prepare time series of full-disk vector magnetic field observations to (2) derive the changing electric field in the solar photosphere over active-region scales. This local electric field is (3) incorporated into a surface flux transport model that reconstructs a global electric field that evolves magnetic flux in a consistent way. These electric fields drive a (4) 3D spherical magnetofrictional (SMF) model, either at high resolution over a restricted range of solid angles or at lower resolution over a global domain to determine the magnetic field and current density in the low corona. An SMF-generated initial field above an active region and the evolving electric field at the photosphere are used to drive (5) detailed magnetohydrodynamic (MHD) simulations of active regions in the low corona. SMF or MHD solutions are then used to compute emissivity proxies that can be compared with coronal observations. Finally, a lower-resolution SMF magnetic field is used to initialize (6) a global MHD model that is driven by an SMF electric field time series to simulate the outer corona and heliosphere, ultimately connecting Sun to Earth. As a demonstration, this report features results of CGEM applied to observations of the evolution of NOAA Active Region 11158 in 2011 February.

日冕全球演化模型 (CGEM) 提供日冕磁场的数据驱动模拟，以更好地了解导致爆发事件的磁能积聚。CGEM 项目开发了六项功能。CGEM 模块 (1) 准备全盘矢量磁场观测的时间序列，以 (2) 在活动区域​​尺度上推导出太阳光球层中不断变化的电场。该局部电场 (3) 并入表面通量传输模型，该模型重建以一致方式演化磁通量的全局电场。这些电场驱动 (4) 3D 球形磁摩擦 (SMF) 模型，在有限的立体角范围内以高分辨率或在全局域上以较低分辨率确定低日冕中的磁场和电流密度。活动区域上方由 SMF 生成的初始场和​​光球层处的演化电场用于驱动 (5) 低日冕活动区域的详细磁流体动力学 (MHD) 模拟。然后使用 SMF 或 MHD 解决方案来计算可以与日冕观测进行比较的发射率代理。最后，使用较低分辨率的 SMF 磁场初始化 (6) 全局 MHD 模型，该模型由 SMF 电场时间序列驱动，以模拟外日冕和日光层，最终将太阳与地球连接起来。作为示范，