太陽閃焰與日冕物質拋射誘發之激震波為太陽高能粒子的主要來源，這些太陽爆發事件的加速粒子自日冕層產生後，可以向下往色球層傳播也可以向外往行星際空間運動。往太陽低層大氣運動的加速粒子主要與閃焰有關，能以影像、頻譜或光譜進行觀測分析，而往行星際空間傳輸的加速粒子則可能來自於閃焰或日冕物質拋射誘發的激震波，能以無線電波動態頻譜圖及現地量測資料分析討論，因此研究太陽大氣的非熱輻射與行星際空間的激震波，將能有助於診斷太陽爆發事件的粒子加速，以及粒子在傳輸過程中所經歷的物理問題。本計畫將利用多波段影像與硬X射線及微波的頻譜資料，結合理論模式，分析非熱電子在太陽大氣傳輸的動力學過程，另一方面將使用太陽風及高能粒子的現地量測資料，結合日冕儀或極紫外影像，分析各類型激震波對粒子加速的貢獻及相對應的太陽爆發源。本計畫以加速粒子連結太陽大氣與行星際空間數個物理問題，屬於跨子領域的研究課題，因此本計畫的研究成果將能提供關於太陽爆發之粒子加速問題多面向的重要參考資訊。 ;Solar flares and coronal mass ejections (CMEs) are two major solar explosions, which are responsible for the production of solar energetic particles. These energetic particles are typically accelerated in the corona and then move downward to the chromosphere or upward to the interplanetary space. The downward motion of energetic particles is mainly flare-associated and can be investigated via imaging and spectral analysis. The energetic particles transport to/in the interplanetary space can come from a flare, a CME-driven shock, or an interplanetary shock, and are usually traced by radio dynamic spectrogram and in-situ measurements. Studying the non-thermal radiations in the solar atmosphere together with the interplanetary shocks will be helpful to diagnose the physical processes of particle acceleration and transport. In this project, we attempt to analyze the dynamics of non-thermal electrons during the transport in the solar atmosphere by combining the images from multiple wavelengths, as well as the hard X-ray and microwave spectra, with the theoretic trap-plus-precipitating model. Moreover, we attempt to investigate the acceleration efficiency of different types of shocks based on the in-situ solar wind and particle measurements and clarify the associated solar eruptive events by comparing with the coronagraph and EUV images. Therefore, this research work is an interdisciplinary study covering solar and interplanetary space. Our research results will provide the significant information on the issue of particle acceleration associated with solar explosions.
