太陽開放磁通區域是高速太陽風主要來源地區。它們是大規模太陽能磁場的主要組成部分，也是極性反轉過程的良好示標。我們之前的研究顯示，相同極性的開放磁通（OMF）區域在太陽活動上升階段，會從一極向赤道遷移，越過赤道，在太陽活動的下降階段期間， 向另一極遷移，導致極性反轉。迄今為止，太陽能發磁機制的模擬和模型還無法完全說明觀察到的開放磁通區域遷移模式。本研究的主要目標是探討OMF地區的形成和變化的物理過程。研究方法是檢查各種OMF特性的統計分佈。物理量的統計分佈與其物理機制有關， 這項研究的結果可以幫助檢查目前OMF的形成機制理論。另一項研究目標是探討OMF和太陽風之間的關係。高速太陽風會導致地磁干擾，目前預測太陽風速是根據一經驗推導得到OMF擴張率和太陽風速度的數學關係， 令人滿意的理論模型或模擬尚未被發展。我們的研究方法是定量比較OMF特性和太陽風特性的統計分佈。其結果可以提供有關驅動太陽風的可能機制的資訊。 ;Solar open magnetic flux regions have been known to be main source regions of high-speed solar wind events that can cause recurrent geomagnetic disturbances. They are a major component of the global coronal magnetic-field structure, and are good tracers of the polarity reversal process of solar magnetic field.Our previous study has revealed that the open magnetic flux (OMF) regions of same polaritymigrate from one pole toward equator during the ascending phase of solar activity, cross the equator, and migrate toward the other pole during the descending phase of the solar activity,leading to the polarity reversal.The main objective of current study is to better understand the physical process of the formation and variation of the OMF regions, and their association with the solar wind.The strategy is to examine the statistical distribution profiles of OMF properties, specifically, the expansion rate, magnetic flux and emission intensity, of individual flux tube.To date, the solar dynamo simulations and models have not completely re-produced the observed OMF migration pattern. Most recent simulations have indicated that small scale processes may play an important role in flux transport and solar dynamo process.Since different statistical distribution profiles are generated by different dynamical processes,the results from this study can help verify the OMF formation mechanism implemented in the current models, and provide useful information for theorists to improve their simulations and models.The prediction of solar wind speed at 1~AU has been based on empirically derived relationship between the expansion rate of OMF and solar wind speed. No satisfactory theoretical models or simulations have been developed to relate the open magnetic field structure to the measured solar wind properties. A quantitative comparison between the distribution profiles of solar wind properties and the profiles of OMF properties can provide information on possible mechanisms that drive the solar wind.
