Energization and Disruption of Magnetic Arcades in the Solar Corona

日冕物质抛射（CME）提供了一个壮观的 太阳活动的表现。等离子体和磁通量 被日冕物质抛射到太阳风中的物质， 地球磁场产生地磁扰动。 计划调查可能的启动机制， CME的。 这将允许检查的假设， 耀斑是单一事件的水雷，理想的或 整体磁结构的电阻不稳定性。 的 调查将围绕着研究的动态 全球日冕场结构的演变（单场和多场 拱廊，以及头盔拖缆配置）作为响应 到剪切光球运动日冕的行为 使用随时间变化的磁流体动力学（MHD）建模 仿真。 日冕磁场的全球演化将是 遵循自洽的球面几何超过几个 太阳半径对光球层运动的响应。 由此产生的等离子体密度和速度的演变将 与现有的CME观测结果进行比较。半隐式方法 将被采用，以允许有效的计算缓慢 日冕磁场中的能量积聚。最初，2- 将使用三维（轴对称）描述， 通过三维模拟和描述的发展。

Coronal mass ejections (CME's) provide a spectacular manifestation of solar activity. The plasma and magnetic flux ejected into the solar wind by CME's subsequently interacts with the Earth's magnetic field to produce geomagnetic disturbances. It is planned to investigate possible initiation mechanisms for CME's. This will permit examination of the hypothesis that CME's and flares are minefistations of a single event, an ideal or resistive instability of the overall magnetic configuration. The investigation will center around a study of the dynamical evolution of global coronal field structures (single and multiple arcades, as well as helmet streamer configurations) in response to shearing photospheric motions. The behavior of the corona will be modelled using time dependent magnetohydrodynamic (MHD) simulations. The global evolution of the coronal field will be followed self-consistently in spherical geometry over several solar radii in response to motions applied at the photosphere. The resulting evolution of the plasma density and velocity will be compared to available CME observations. Semi-implicit methods will be employed to allow for efficient computation of slow energy build-up in the coronal magnetic fields. Initially, a 2- dimensional (axisymmetrical) description will be used, followed by development of a 3-dimensional simulation and description.