一般而言，太陽閃焰在日冕層釋放的能量，可經由熱傳導效應或伴隨閃焰產生的非熱電子傳輸至較低層大氣，造成色球層局部區域的電漿加熱，進而發生熱電漿向上運動的色球蒸散現象，因此分析閃焰期間色球層電漿的反應情形，將能有助於釐清閃焰各階段的能量傳輸問題。本計畫將利用IRIS衛星的譜線資料及觀測影像，結合RHESSI衛星的硬X射線影像或頻譜資料、及SDO衛星的AIA多波段影像，分析不同色球蒸散類型的色球層譜線反應，探討因非熱電子所觸發的色球層加熱現象的譜線特性，並量化其與閃焰非熱輻射的相關性。對於太陽閃焰非熱輻射研究而言，本計畫預期將提出一種極為關鍵的新診斷方式，而本計畫的研究成果亦將能對閃焰能量傳輸議題提供重要的參考資訊。 ;It is generally accepted that the released energy in the corona during solar flares is transported downward to the lower atmosphere via thermal conduction or flare-generated non-thermal electrons, leading to the plasma heating at the local regions of chromosphere. The upward motion of heated plasma is expected to occur subsequently, which is the so-called chromospheric evaporation. Investigating the response of chromospheric plasma during flares is helpful to clarify the energy transport processes in different flaring phases. In this project, we attempt to analyze the chromospheric emission lines, characterize the spectral parameters for the chromospheric heating driven by non-thermal electrons, and quantify the correction between the derived parameters and flare non-thermal emissions by combining the IRIS spectral measurements with the RHESSI hard X-ray and SDO/AIA multi-wavelength observations. This research work will propose a new method to diagnose the flare non-thermal emissions and the associated results can provide the significant information on the energy transport issue in solar flares.
