太陽的差動自轉(solar differential rotation)可將原本南北方向的磁
偶極場(poloidal field)拉成東西方向(toroidal field)。因此太陽差動自轉
在太陽磁場的週期變化中，扮演著很重要的角色。早期科學家從追踨
太陽黑子(sunspots)的運動所得到的太陽差動自轉模式受到太陽黑子
分佈情形的限制，在時空解析度上，很難再進一步提升。台灣日震觀
測網(Taiwan Oscillation Network, TON)提供一分鐘一張高時空解析度
的broadband K-line image。這些K-line 影像圖中除了太陽黑子與明亮
的譜斑(plages) 外還有超米粒組織的明亮邊界(supergranulation
boundaries，SGB)，都可以作為研究太陽差動自轉的追蹤標記。由於
超米粒組織的明亮邊界的緯度分佈甚廣且數量不受太陽週期的影
響，因此藉著分析TON K-line image 可得高時空解析度之太陽表面差
動自轉的情形。
在本論文的研究中，我們從1994 年起，每年分析數日已經
remapped 的TON 資料來研究太陽差動自轉隨太陽週期的變化情形。
初步的結果發現，在1994~2000 年間，太陽的轉速在北半球，有逐年
減慢的趨勢，但在南半球，則是逐年的增快。但是進一步的檢驗
remapped 的資料後，發現有一部分的南北不對稱性是受到不正確的
remapped 影像的影響。因此本論文在太陽差動自轉隨太陽週期變化
方面的研究仍未成功。但是在本研究中，我們設計了一種只要半天的
資料量，就可以很快的求得太陽在不同緯度的自轉角速率。我們同時
找到一種檢驗remapped 結果是否正確的方法。相信我們所研發的這
兩項資料分析方法，將對未來利用TON 資料做日震分析的研究有很
大的幫助。
i

Solar latitudinal differential rotation, which can generate toroidal
magnetic field from a poloidal magnetic field, plays an important role on
solar dynamo and formation of solar cycle. Solar differential rotation
was first found by tracing sunspots'' motion. The well-known solar
differential rotation formula obtained from sunspots'' motion is only
applicable to the middle- and lower- latitude regions and has a poor
latitudinal resolution during solar minimum. Supergranulations, or
chromosphere networks, or plages are excellent targets for studying solar
differential rotation in all latitudes and during different phases of solar
cycle. The one-minute broadband K-line images obtained from Taiwan
Oscillation Network (TON) provide an opportunity to study differential
rotation of supergranulations or plages up to very high latitude.
Our preliminary results show that weak north-south asymmetry on
solar differential rotation is found during years 1994~1997. Strong
north-south asymmetry on solar differential rotation is found during years
1998~2000. According to our preliminary study, solar rotation rate
decreases with time in northern hemisphere, but increases with time in
southern hemisphere during years 1994~2000. However, further study
indicates that the strong north-south asymmetry on solar differential
rotation may partially due to incorrect mapping of the TON data sets we
used in this thesis. Thus, our study of solar cycle dependence on solar
differential rotation is not fully successful. But, in this thesis we have
developed a very efficient way to obtain solar rotation rate at different
latitude. We have also found a simple way to check and to improve the
accuracy of a remapped image. Therefore, using the techniques
developed in this thesis can provide accurate remapped images and
real-time solar differential rotation information for future solar
seismology study using TON data sets.

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