SHINE: Linking Flare Radiation to the Dynamics of Coronal Mass Ejections

本文将建立一个耦合模型来解释太阳日冕物质抛射（CME）的大尺度动力学和相关耀斑环状结构辐射的小尺度能量学。通常应用于回路的传统特设加热函数将被基于CME开始和初始演化确定的参数的解析模型所取代。这一努力使得将耀斑环的温度和动力学与日冕物质抛射的传播和演化联系起来成为可能。因为它必须同时考虑日冕物质抛射和耀斑的观测，这个耦合模型将受到严重的限制，并可能被太阳观测校准。如果该模型在这方面被证明是成功的，它可以用来预测cme的性质，例如，它们的速度和嵌入磁场的强度，从相关的耀斑辐射的特征。

A coupled model which accounts for the large-scale dynamics of a solar coronal mass ejection (CME), and the small-scale energetics of the radiation from associated flaring loop-like structures will be developed. The conventional ad hoc heating function usually applied to the loops will be replaced with an analytical model based on parameters determined from the onset and initial evolution of the CME. This effort makes it possible to relate the temperature and dynamics of flare loops to the propagation and evolution of CMEs. Because it will have to account simultaneously for both the CME and flare observations, this coupled model will be severely constrained and potentially calibrated by solar observations. If the model turns out to be successful in this regard, it could be used to forecast the properties of the CMEs, e.g., their speed and the strength of the embedded magnetic field) from the characteristics of the associated flare radiation.