磁層頂日下點對峙距離和行星際磁場錐角值關係的研究

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姓名

黃昭維(Chao-Wei Huang) 查詢紙本館藏

畢業系所

太空科學研究所

論文名稱

磁層頂日下點對峙距離和行星際磁場錐角值關係的研究
(A Comprehensive Study of Relationship Between Subsolar Standoff Distance of the Magnetopause and Cone Angle of Interplanetary Magnetic Field)

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摘要(中)

太陽風和地球磁層交互作用的過程中，磁層頂日下點對峙距離是一項重要的參數，其值主要由行星際磁場的Z方向分量 (Bz)和太陽風動壓 (Dp)所控制，但也與行星際磁場錐角有關，先前的研究發現行星際磁場錐角值小時，亦即行星際磁場幾乎平行日地連線時，日下點對峙距離值會較大。日下點對峙距離和行星際磁場錐角值在不同的太陽風條件下的關係至今並未被系統地討論。從西蜜斯(Time History of Events and their Macroscopic Interactions during Substorms, THEMIS)的衛星資料庫判斷日下點附近的磁層頂的磁層頂穿越事件，再由OMNI資料庫選取相對應的太陽風條件資料，然後利用這些事件，區分成南向行星際磁場與北向行星際磁場和太陽風高動壓與低動壓情況。我們發現日下點對峙距離和行星際磁場錐角值的關係會隨著行星際磁場的Z方向分量和太陽風動壓改變，在南向行星際磁場和高動壓時，發現行星際磁場錐角接近90度時有最小的日下點對峙距離值。

摘要(英)

The subsolar standoff distance of the Earth’s magnetopause is an important parameter in studying interactions between the solar wind and the magnetosphere. Its value is mainly controlled by the north-south component (Bz) of the interplanetary magnetic field (IMF) and solar wind dynamic pressure (Dp). Recent studies have found that the subsolar standoff distance is large for small cone angle of the IMF, that is, the orientation of the IMF is almost parallel to the Sun-Earth line. However, relationship between the subsolar standoff distance and cone angle under different IMF Bz and Dp conditions have not been comprehensively studied. With a large set of subsolar magnetopause crossings identified from the THEMIS data and their corresponding solar wind conditions obtained from the OMNI data, we are able to bin the magnetopause crossings in four categories by the southward and northward polarities of the IMF, and large and small Dp. Here we find that the relationship between the subsolar standoff distance and cone angle changes with IMF Bz and Dp. The smallest subsolar standoff distance occurs when the cone angle is near 90 degrees in the category of southward IMF and high Dp.

關鍵字(中)

★ 磁層頂日下點對峙距離
★ 行星際磁場錐角值

關鍵字(英)

★ IMF cone angle
★ Subsolar standoff distance

論文目次

中文摘要 ................................................ I
英文摘要 ............................................... II
誌謝 .................................................. III
目錄 ................................................... IV
圖目錄 ................................................ VII
表目錄 .................................................. X
符號說明 ............................................... XI
一、緒論 .......................................... 1
1-1 簡介 .......................................... 1
1-2 太空環境介紹 .................................. 1
1-3 研究動機及目的 ................................ 2
1-4 論文架構 ...................................... 3
二、理論背景介紹 .................................. 4
2-1 磁層介紹 ...................................... 4
2-2 磁層頂位置 .................................... 5
2-3 太陽風動壓經過磁鞘的壓力轉換 ................. 12
2-4 早期磁層頂模式介紹 ........................... 13
2-5 影響日下點對峙距離的參數 ..................... 16
2-6 磁場線重聯效應 ............................... 17
2-7 行星際磁場錐角 ............................... 21
三、資料處理方法.................................. 23
3-1 衛星介紹 ..................................... 25
3-2 衛星資料ASCII檔案轉換成SAVE檔案 .............. 28
3-3 判斷磁層頂穿越 ............................... 29
3-4 斷磁層頂穿越對應太陽風參數選取 ............... 30
3-5 Aberration效應................................ 31
3-6 日下點資料挑選 ............................... 33
3-7 磁層頂穿越事件的空間分佈 ..................... 34
四、資料分析 ..................................... 37
4-1 所有事件 ..................................... 39
4-2 南向和北向行星際磁場事件 ..................... 41
4-3 太陽風高動壓和低動壓事件 ..................... 43
4-4 北向和南向行星際磁場，太陽風高動壓和低動壓事件 45
五、討論與結論 ................................... 49
5-1 分析討論 ..................................... 53
5-2 未來工作 ..................................... 53
5-3 結論 ......................................... 56
參考文獻 ............................................... 57
附錄一磁層頂穿越事件清單 .............................. 61

參考文獻

Aubry, M. P., C. T. Russell, and M. G. Kivelson (1970), Inward Motion of the Magnetopause before a Substorm, J. Geophys. Res., 75(34), 7018–7031, doi:10.1029/JA075i034p07018.
Baumjohann, W., G. Paschmann, and C. A. Cattell (1989), Average plasma
properties in the central plasma sheet, J. Geophys. Res., 94, 6597.
Boardsen, S. A., T. E. Eastman, T. Sotirelis, and J. L. Green (2000), An Empirical Model of the High-latitude Magnetopause, J. Geophys. Res., 105(A10), 23,193–23,219, doi:10.1029/1998JA000143.
Boudouridis, A., L. R. Lyons, E. Zesta, and J. M. Ruohoniemi (2007), Dayside reconnection enhancement resulting from a solar wind dynamic pressure increase, J. Geophys. Res., 112, A06201, doi:10.1029/2006JA012141.
Borovsky, J. E., M. Hesse, J. Birn, and M. M. Kuznetsova (2008), What determines the reconnection rate at the dayside magnetosphere?, J. Geophys. Res., 113, A07210, doi:10.1029/2007JA012645.
De Keyser, J., and M. Roth (1998), Magnetic field rotation at the dayside magnetopause: AMPTE/IRM observations, J. Geophys. Res., 103, 6663.
Dušik, Š., G. Granko, J. Šafrankova, Z. Němeček, and K. Jelinek (2010), IMF cone angle control of the magnetopause location: Statistical study, Geophys. Res. Lett., 37, L19103, doi:10.1029/2010GL044965.
Formisano, V., V. Domingo, and K.‐P. Wenzel (1979), The threedimensional shape of the magnetopause, Planet. Space Sci., 27, 1137– 1149, doi:10.1016/0032-0633(79)90134-X.
Fairfield, D. H., R. P. Lepping, E. W. Hones, S. J. Bame, and J. R. Asbridge (1981), Simultaneous measurements of magnetotail dynamics by IMP spacecraft, J. Geophys. Res., 86, 1396.
Howe, H. C., Jr., and J. H. Binsack (1972), Explorer 33 and 35 plasma observations of magnetosheath flow, J. Geophys. Res., 77(19), 3334–3344,
doi:10.1029/JA077i019p03334.
Kivelson, M. G. and C. T. Russell, Introduction to Space Physics, Cambridge University Press, 1995.
Kawano, H., S. M. Petrinec, C. T. Russell, and T. Higuchi (1999), Magnetopause shape determinations from measured position and estimated flaring angle, J. Geophys. Res., 104(A1), 247–261, doi:10.1029/98JA02479.
Lennartsson, W., and E. G. Shelley (1986), Survey of 0.1 to 16 keV/e
plasma sheet ion composition, J. Geophys. Res., 91, 3061.
Lopez, R. E., M. Wiltberger, S. Hernandez, and J. G. Lyon (2004), Solar wind density control of energy transfer to the magnetosphere, Geophys. Res. Lett., 31, L08804, doi:10.1029/2003GL018780.
Li, W., J. Raeder, M. Oieroset, and T. D. Phan (2009), Cold dense magnetopause boundary layer under northward IMF: Results from THEMIS and MHD simulations, J. Geophys. Res., 114, A00C15, doi:10.1029/2008JA013497
Lin, R. L., X. X. Zhang, S. Q. Liu, Y. L. Wang, and J. C. Gong (2010), A three-dimensional asymmetric magnetopause model, J. Geophys. Res., 115, A04207, doi:10.1029/2009JA014235.
Onsager, T. G., J. D. Scudder, M. Lockwood, and C. T. Russell (2001), Reconnection at the high-latitude magnetopause during northward interplanetary magnetic field conditions, J. Geophys. Res., 106, 25,467.
Ober, D. M., M. F. Thomsen, and N. C. Maynard (2002), Observations of bow shock and magnetopause crossings from geosynchronous orbit on 31 March 2001, J. Geophys. Res.,107(A8), 1206, doi:10.1029/2001JA000284.
Petrinec, S. M., P. Song, and C. T. Russell (1991), Solar cycle variations in the size and shape of the magnetopause, J. Geophys. Res., 96(A5), 7893– 7896, doi:10.1029/90JA02566.
Petrinec, S. M., and C. T. Russell (1995), An Examination of the Effect of Dipole Tilt Angle and Cusp Regions on the Shape of the Dayside Magnetopause, J. Geophys. Res., 100(A6), 9559–9566, doi:10.1029/94JA03315.
Petrinec, S. M., and C. T. Russell (1996), Near‐Earth magnetotail shape and size as determined from the magnetopause flaring angle, J. Geophys. Res., 101(A1), 137–152, doi:10.1029/95JA02834.
Roelof, E. C., and D. G. Sibeck (1993), Magnetopause shape as a bivariate function of interplanetary magnetic field Bz and solar wind dynamic pressure, J. Geophys. Res., 98(A12), 21,421–21,450, doi:10.1029/ 93JA02362.
Sibeck, D. G., R. E. Lopez, and E. C. Roelof (1991), Solar wind control of the magnetopause shape, location, and motion, J. Geophys. Res., 96(A4), 5489–5495, doi:10.1029/90JA02464.
Shue, J.-H., Pressure Conversion in the Solar Wind-Magnetosphere Interaction, American Geophysical Union, Fall Meeting 2010, abstract #SM51B-1779
Shue, J.-H., J. K. Chao, H. C. Fu, C. T. Russell, P. Song, K. K. Khurana, H. J. Singer (1997), A new functional form to study the solar wind control of the magnetopause size and shape, J. Geophys. Res., 102(A5), 9497-9512, 10.1029/97JA00196.
Shue, J.-H., P. Song, C. T. Russell, J. T. Steinberg, J. K. Chao, G. Zastenker, O. L. Vaisberg, S. Kokubun, H. J. Singer, T. R. Detman, H. Kawano (1998), Magnetopause location under extreme solar wind conditions, J. Geophys. Res., 103(A8), 17691-17700, 10.1029/98JA01103.
Shue, J.-H., et al. (2011), Uneven compression levels of Earth's magnetic fields by shocked solar wind, J. Geophys. Res., 116, A02203, doi:10.1029/2010JA016149.
Shevyrev, N. N., G. N. Zastenkera, and J. Du (2007), Statistics of lowfrequency variations in solar wind, foreshock and magnetosheath: INTERBALL-1 and CLUSTER data, Planet. Space Sci., 55(15), 2330 –2335.
Suvorova, A. V., J.-H. Shue, A. V. Dmitriev, D. G. Sibeck, J. P. McFadden, H. Hasegawa, K. Ackerson, K. Jelinek, J. Šafrankova, and Z. Němeček (2010), Magnetopause expansions for quasi-radial interplanetary magnetic field: THEMIS and Geotail observations, J. Geophys. Res., 115, A10216, doi:10.1029/2010JA015404.
Taiwan THEMIS website, http://themis.ss.ncu.edu.tw
Wikipedia, http://en.wikipedia.org
陳怡璇 (2009)，太陽風對地球磁層頂內側磁場之影響，國立中央大學太空科學研究所
莊博硯 (2007)，磁層頂位置之不對稱性研究，國立中央大學太空科學研究所

指導教授

許志浤(Jih-Hong Shue)

審核日期

2011-7-1

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