日冕洞是太陽磁場規模最大的區域，並且是高速太陽風的主要來源地區。它們的位置和面積對於研究太陽及行星際磁場，以及預測可能影響地球的高速太陽風非常重要。因此，準確辨識日冕洞的位置和面積相當重要。太陽面上的日冕洞通常有兩種辨識方法: (1)具有開放磁力線的區域（OMF), 或 (2)主要是單極磁場的低日冕幅射區域（LIR）。但是，用兩種方法辨識的日冕洞並不總是彼此重合。我們之前的研究顯示，只有12％的OMF地區位於LIR內。差異是來自於高日冕幅射的OMF地區 (或亮的OMF地區），以及具有封閉磁場線結構的LIR區域。觀測到的日冕幅射與磁場環境中電漿能量傳輸及產生 的過程有關。因此，OMF和LIR日冕洞之間的不一致，可能是由於在兩種日冕洞辨識方法中，對於日冕幅射與磁場結構之間的關係不正確的假設所造成。本研究的目的是研究磁場結構對日冕洞幅射的影響，並改善兩種辨識方法以期減少兩種日冕洞之間的不一致。 ;Coronal holes are the regions with largest scale solar magnetic fields, and are major source regions of high speed solar wind streams (HSSS). Their locations and areas are important for tracing the global magneticfields, modelling the heliospheric magnetic fields, andpredicting the HSSS events that may impact the Earth.Accurate identification of the coronal holes is thus important for various studies. The on-disk coronal holes are often identified either as the regions with open magnetic field lines (OMF) or as the regions with low coronal emission and predominantly unipolar magnetic fields (LIRs). The coronal holes identified by the two methods, however, do not always coincide with each other.Our previous study showed that only 12\% of the OMF regions are located within LIRs. The discrepancy comes from the OMF regions with high coronal emission and from the LIR regions with closed magnetic-field line structures. The emission of coronal plasma is the result of energy transport and generation of plasma in a magnetic field environment. Therefore, the inconsistency between OMF and LIR coronal holes is likely due to inaccurate presumptions of the relationship between the coronal emission and magnetic field structure in the two coronal-hole identification methods. The objective of this proposal is to investigate the effects of magnetic field on the coronal emission of coronal holes and to improve the two coronal hole identification methods to reduce the inconsistency between the coronal holes determined by them.