Magnetic Effects in the Sun's Corona and Interior

太阳磁场在时间上是周期性的， 在太空中断断续续。 该领域发挥着基础作用， 太阳炽热的外日冕的形成， 年活动周期。这项研究将探讨磁 太阳上的现象，从探测内部磁场 利用日震学来研究 日冕，包括波的产生和 太阳耀斑中粒子的加速 日震学 研究将有助于阐明结构和时间 太阳内部磁场的行为。 的 日冕磁场演化研究将集中于 奇点的形成和平衡的丧失， 这对于理解稳态日冕 加热和喷发现象，如耀斑和物质抛射。 粒子加速研究将集中在产生 耀斑过程中的磁流体扰动， 粒子与这些波相互作用的模拟。 后者 应适用于各种加速， 除了太阳耀斑外，分析和 将采用基于先前研究的数值技术。

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.