Solar coronal active region dynamic 3D modelling

启动太阳日冕活动区三维建模：即活动区加热挑战，类似于地球环境建模或牛顿磁重联挑战。我们的目标是识别AR磁能释放的关键机制，使用磁流体动力学，多流体和动力学数值代码与磁场取自ATST和SDO HMI magetogram数据，并使用基于绿色函数算法的三维位场外推。这应该给我们一个深入了解波耗散与重连日冕加热的辩论。Tsiklauri D.的进一步细节，“太阳拼图中缺失的部分”，Atronomy & Geophyisics，第50卷，第5期，pp。5.32-5.38（2009年）。该项目将广泛使用QMUL和DiRAC HPC设施，并且是非常数据和CPU密集型的。

Initiation of solar coronal active region 3D modelling: i.e. Active Region (AR) heating challenge in analogy with Geo-Environmental Modelling (GEM) or Newton magnetic reconnection challenges. The goal is to identify the key mechanisms of AR magnetic energy reslease using MHD, multi-fluid and kinetic numerical codes with magnetic fields taken from ATST and SDO HMI magetogram data and using 3D potential field extrapolations based on Green's function algorithm. This should give us an insight into wave dissipation versus reconnection coronal heating debate. Further details in Tsiklauri D., "Missing pieces of the solar jigsaw puzzle", Atronomy & Geophyisics, Volume 50, Issue 5, pp. 5.32-5.38 (2009). The project will have exte4nsive use of QMUL and DiRAC HPC facilities and is very data- and CPU- intensive.