Theoretical Studies of Solar Flares and Active Regions

本文将通过理论研究来了解 磁场和电流系统在太阳耀斑中的作用， 并了解等离子体流与辐射的相互作用 在耀斑和活动区的色球层和日冕中。 具体而言，这项工作将进一步发展一种分析 在X型中性点处的磁重联的描述， 并将研究扩展到数值模拟， 气压对光球磁场影响 从矢量磁图推断;使用活动区域磁 场模型，以确定横截面积变化沿着 用于流体动力学和粒子研究的日冕环; 改进耀斑渐变阶段演化的模型， 这将复杂的流体动力学描述简化为简单的 常微分方程，模拟整个 火炬可行;将类似技术应用于热研究 稳定的活动区循环;和开发一个新的，更简单的; 更快的，辐射流体动力学代码的研究的脉冲 色球耀斑这些问题将用解析法来研究 以及应用于气体动力学、辐射 转移和磁流体动力学方程。 这项工作将有助于 在解释光谱数据和矢量磁图， MAX '91期间的地面光学望远镜。***

This theoretical research will be conducted to understand the role of magnetic fields and current systems in solar flares, and to understand the interaction of plasma flows with radiation in both the chromosphere and corona of flares and active regions. Specifically, this effort will further develop an analytic description of magnetic reconnection at an X-type neutral point, and extend the studies to numerical simulation; study the influence of gas pressure on photospheric magnetic fields as inferred from vector magnetograms; use active region magnetic field models to determine cross-sectional area variation along coronal loops for use in hydrodynamic and particle studies; improve a model for the evolution of the gradual phase of flares, which reduces the complex hydrodynamic description to a simple ordinary differential equation, making simulations of the entire flare feasible; apply similar techniques to studies of thermal stability of active region loops; and develop a new, simpler; faster, radiation-hydrodynamics code for studies of the impulsive chromospheric flare. These problems will be studied with analytic and numerical techniques applied to the gasdynamic, radiation transfer, and magnetohydrodynamic equations. This work will aid in interpreting spectroscopic data and vector magnetograms from ground based optical telescopes during MAX '91. ***