太陽風將太陽表面的磁場帶出來，因為太陽自轉的緣故，使得磁場在行星際空間呈現阿基米得螺旋狀的扇形邊界(sector boundary)，部分學者認為太陽閃焰(Flare)爆發產生後會以爆炸波的方式傳向行星際空間,這個波會穿越扇形邊界，也有部分學者認為Coronal Mass Ejections，(簡稱CMES)所帶出來的電漿物質會去推擠扇形邊界，但卻無法穿越邊界，僅會與扇形邊界產生交互作用，在其前面會產生震波,使得扇形邊界產生變形並推擠其前進。所以我們就以Hakamada-Akasofu-Fry Code (以kinematic為基礎的code) 去模擬，並比較實際WIND衛星觀測資料，我們用1998年2月14日，1998年5月2日，2000年5月22日及2000年11月25日這些CMES暴發事件，由分析研究結果發現，CMES會推擠扇形邊界，造成形狀的改變，因此也產生了行星際震波到逹時間(Arrival time)與假設沒有CME的情況下所到達的時間差異很大，此類的差異以Halo CMES尤其顯著。由我們的分析結果，發現大部份的震波是被物質所推擠前進的，而且從CMES與扇形邊界交互作用的結果,我們認為行星際震波並非源自於太陽閃焰爆發所產生,而是由於CME所造成的。

Solar wind carries the frozen magnetic field from the solar surface into interplanetary space, making a shape of Archimedes spiral due to the rotation of the sun. The sector boundary is identified at the region when large scale polarity changes are located.Some scientists believe that a shock wave generated by a large flare does not effect the sector boundary after its transmission. But some scientists consider coronal mass ejections (CMES) as a group of high energy plasmas which comes out from the sun, a shock may form in front of it due to the interaction of the shock and its following material with the sector boundary. The shock interacts with the sector boundary will change the shape of the sector boundary substantially. In order to demonstrate which of the above hypothesis is correct, We used the kinematic approach of the Hakamada-Akasofu-Fry code to simulate some solar interplanetary events occurred during 1998 Feb 14, 1998 May 2, 2000 May 22, 2000 Nov 25. Our analysis shows that the arrival times of the shock and the sector boundary were correct predicted from the HAF code which is different from an undisturbed sector boundary for a free propagation shock as suggested by Flare-caused theory.

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