Magnetic Effects in the Sun's Corona and Interior

太阳磁场在时间上是周期性的，在空间上是间歇性的。这个磁场在太阳炽热的外冕的形成和二十二年的活动周期中起着基本的作用。这项研究将研究太阳上的磁现象，范围从使用日震学探测内部场到研究日冕中场的演变，包括太阳耀斑中波的产生和粒子的加速。日震学研究将有助于阐明太阳内部磁场的结构和时间行为。日冕磁场演化的研究将集中于奇点的形成和平衡的丧失，这对于理解稳态日冕加热和耀斑和物质抛射等爆发现象都是重要的。粒子加速研究将侧重于耀斑过程中流体磁扰动的产生，以及粒子与这些波相互作用的模拟。除太阳耀斑外，后者还应适用于各种环境中的加速。将采用基于先前研究的分析和数值技术。

The solar magnetic field is cyclical in time and intermittent in space. The field plays a basic role in the formation of the Sun's hot outer corona and in the twenty two year activity cycle. This study will investigate magnetic phenomena on the Sun which range from probing the interior field using helioseismology to studying the evolution of the field in the corona, including the generation of waves and the acceleration of particles in solar flares. The helioseismology studies will help to elucidate the structure and temporal behavior of the magnetic field in the solar interior. The investigation of coronal magnetic field evolution will focus on the formulation of singularities and the loss of equilibrium, which are important for understanding both steady state coronal heating and eruptive phenomena such as flares and mass ejections. The particle acceleration studies will focus on the generation of hydromagnetic disturbances during the flare process and on simulations of particle interaction with these waves. The latter should have application to acceleration in a wide range of environments in addition to solar flares. Both analytical and numerical techniques based on prior studies will be employed.