日冕拋射物質對扇形邊界的影響

以作者查詢圖書館館藏

、以作者查詢臺灣博碩士

、以作者查詢全國書目

、勘誤回報

、線上人數：13

、訪客IP：3.22.51.241

姓名

柳文冠(Wean-Kuan Leau) 查詢紙本館藏

畢業系所

太空科學研究所

論文名稱

日冕拋射物質對扇形邊界的影響
(Interaction between the Solar Coronal Mass Ejections and Heliospheric Sector Boundary)

相關論文

★ 日側磁層頂在同步軌道附近對強烈太陽風的反應情形

★ Fast Magnetosonic Shocks in the interplanetary Space and Magnetosphere

檔案

[Endnote RIS 格式]

[Bibtex 格式]

[相關文章]

[文章引用]

[完整記錄]

[館藏目錄]

[檢視]

[下載]

本電子論文使用權限為同意立即開放。
已達開放權限電子全文僅授權使用者為學術研究之目的，進行個人非營利性質之檢索、閱讀、列印。
請遵守中華民國著作權法之相關規定，切勿任意重製、散佈、改作、轉貼、播送，以免觸法。

摘要(中)

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。

摘要(英)

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.

關鍵字(中)

★ 日冕拋射物質
★ 扇形邊界

關鍵字(英)

★ coronal mass ejections
★ sector boundary

論文目次

摘要
誌謝
本文目錄
圖目錄
表目錄
第一章緒論
1.1 研究動機 1
1.2 研究目的 3
第二章太陽與行星際結構
2.1 太陽結構 5
2.2 太陽活動 8
2.3 日冕結構 10
2.4 行星際磁雲 11
2.5 太陽風 11
第三章 Hakamada-Akasofu-Fry Code
3.1 簡介 26
3.2模擬程式介紹 31
第四章實驗過程及結果
4.1 模擬事件 37
4.2 實驗結果 37
第五章分析討論與總結
5.1 數據分析統計 49
5.2 未來可能的發展與改進 50
5.3 總結 52
附表 55
參考文獻 60

參考文獻

Akasofu, S.I., Predicting geomagnetic Stroms As A Space Weather Project, In American Geophysical Union Geophysical Monograph, Washington DC, in press.2001.
Akasofu, S.I., predicting Geomapnetic Storms as a space weather project cospar colloquia series Vol12. P3-20 space weather study using multipoint techriques, Perganom,2002.
Athay, R.G. and O.R.White,Chromospheric and coronal heating by sound wave, Astro-phys. J., 226, 1135.1976.
Burlag, L.F., R.M.Skoug, C.W.Smith,D.F.Webb,T.H.Zurbuchen, and Alysha Reinard,Fast ejecta during the ascending phase of solar cycle 23, Journal of Geophysical research, vol 106, No.A10,p. 20957-20977,October 1, 2001.
Burlaga,L.F.,Magnetic clouds,in Physics of the Inner Heliosphere,vol2,edited by R.Schwenn and E.Marsch,Springer-Verlag,New York,1991.
Burlaga, L.F.,S.P. Plunkett, O.C. St. Cyr, Successive CMES and complex ejecta, J.Geophys. Res., Vol 107, 1266, 2002.
Chao, J.K. and H.H.Chen, Prediction of Southward IMF Bz in space weather: Progress and challenges in research and application, Geophysical monograph 125, space weather, P183-189,2001.
Dryer, M., C.D.Fry, W.Sun, C.Deehr, Z.Smith, S.I.Akasofu, and M.d.Andrews.Solar Physics 204: 267-286,2001.
Fry, C.D., M.Dryer,Z.smith, W.Sun,C.S. Deehr, and S.I.Akasofu. Forecasting solar wind structures and shock arrival times using an ensemble of models.JGR,vol 108,no.A2,1070,2003.
Fry, C.D., W.Sun, C.S.Deehr, M.Dryer, Z.Smith, S-I Akasofu, M.Tokumaru, and M.Kojima, Improvements to the HAF solar wind model for space weather predictions, Journal of Geophysical research, vol 106, No. A10,pages 20, 985-21,001, octorber 1,2001.
Gopalswamy, N., A.Lara, M.L.Kaiser, and J-L. Bougeret, Near-Sun and near-Earth manifestations of solar eruptions, Journal of Geophysical research, vol. 106, No. A11, pages 25,261-25,277,November 1,2001.
Gosling, J.T. , and D.T. McComas, Field line draping about fast coronal mass ejecta; A source of strong out-of-eclipitc interplanetary magnetic field, Geophys. Res. Lett, 14,355,1987.
Gosling,J.T., Cornal mass ejections : An overview, Cornal mass ejections, Geophysical monograph 99, the American Geophysical Union, 1997.
Hakamada, K., and S.-I. Akasofu. Simulation of Three-Dimensional solar wind Disturbances, space science Reviews 31,P3-70,1982.
Hu,Y.Q., X.Z. Jia, Interplanetary shock interaction with the heliospheric current shect and its associated structures, J.Geophy. Res., 106, 29299-29304,2001.
Hundhausen, A.J., Coronal Expansion and Solar Wind, Springer-Verlag, New York, 1972.
Kivelson, M. G., Christopher T., Russdl, Introduction to space physics,p59, Cambridge University press 1995.
Parker, E.N., Theoretical studies of the solar wind phenomena, Astrophys. J., 128,664,1958.
Parker,E.N.,Interplanetary dynamical processes, Interscience, New York, 1963.
Priest, E.R., Solar magneto-hydrodynamics, D.Reidel Publishing Company, 1943.
Schwenn, R., The average solar wind in the inner heliosphese : Structure and slow variations, in Solar Wind Five, NASA Conf. Publ. CP-2280, 489, 1983.
Smith, Z.,C.S.Deehr, Performance of interplanetary shock prediction models STOA and ISPM,J. Atmos. So1. Terr. Physics, 62,1265-1274,2000.
Sun,W., and S.I. Akasofu, Calibration of the kinematic method of studying solar wind disturbances on the basis of a one-dimension MHD solution and a simulation study of the heliosphere disturbances between 22 November and 6 December 1977. Plant. Space Sci. Vol 33.No.8,pp.933-943,1985.
Tsurutani,B. W.D.Gonzalea,F.Tang, Origin of Interplanetary Southward Magnetic Fields Responsible for Major Magnetic Storms Near Solar Maximum, JGR P8519-8531, Aug 1, 1988.
Webb, D. F., E.W. Cliver, N.U.Crooker, O.C. St.Cyr, and B.J. Thompson, Relationship of halo coronal mass ejections, magnetic cloud, and magnetic storms, J. Geophys. Res., 105,7491-7508,2000.
Whang, Y.C., Conversion of magnetic field energy into kinetic energy in the solar wind, p. 236, National Aeronaulics and Space Administration, Washington, 1972.
Wright, C.S., and L.F. McNAMARA, The Relationships between Disappearing Solar Filaments, Coronal Mass Ejections, and Geomagnetic Activity, Solar Phys, 87,401-417,1983.
Zhang, G. and L.F. Burlaga, Magnetic clouds, Geomagnetic Disturbances and Cosmic Ray Decreases, J. Geophys. Rev., 93,2511-2518,1988.

指導教授

趙寄昆(Jih-Kwan Chao)

審核日期

2004-1-14

推文