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1 ＩｎｔｒｏｄｕｃｔｉｏｎＴｈｅｐｏｌａｒｒｅｇｉｏｎｉｓａｎｉｍｐｏｒｔａｎｔａｒｅａｆｏｒｅｎｅｒｇｅｔｉｃｃｏｕｐｌｉｎｇｂｅｔｗｅｅｎｓｏｌａｒｗｉｎｄａｎｄｅａｒｔｈ’ｓｍａｇｎｅｔｏｓｐｈｅｒｅ .Ｔｈｅｃｕｓｐｉｓｔｈｅｄｉｒｅｃｔｐａｔｈｆｏｒｓｏｌａｒｗｉｎｄｐｅｎｅｔｒａｔｉｎｇｉｎｔｏｔｈｅｍａｇｎｅｔｏｓｐｈｅｒｅｏｒｅｖｅｎｉｎｔｏｔｈｅｉｏｎｏｓｐｈｅｒｅａｎｄｉｔａｌｓｏｉｓａｃｏｎｖｅｒｇｅｎｔｒｅｇｉｏｎｆｏｒａｌｏｔｏｆｍａｇｎｅｔｏｓｐｈｅｒｉｃｂｏｕｎｄａ… 相似文献
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Inter-hemispheric comparisons of geospace environment in the polar regions—A proposed cooperative research program between China and Norway 总被引：1，自引：0，他引：1
1 ＩｎｔｒｏｄｕｃｔｉｏｎＧｅｏｓｐａｃｅｄｅａｌｓｗｉｔｈｔｈｅＥａｒｔｈ’ｓｍｉｄｄｌｅａｎｄｕｐｐｅｒａｔｍｏｓｐｈｅｒｅ ,ｔｈｅｒｍｏｓｐｈｅｒｅ/ｉｏｎｏ ｓｐｈｅｒｅａｎｄｍａｇｎｅｔｏｓｐｈｅｒｅ .Ｔｈｉｓ“ｇｅｏｓｐａｃｅｅｎｖｉｒｏｎｍｅｎｔ”ｉｓｏｆｇｒｅａｔｓｃｉｅｎｔｉｆｉｃａｎｄｐｒａｃｔｉ ｃａｌｉｎｔｅｒｅｓｔ,ｐａｒｔｉｃｕｌａｒｌｙａｓｉｔｉｓｏｆｔｅｎｓｕｂｊｅｃｔｔｏｄｉｓｔｕｒｂａｎｃｅｓ.Ａｂｌａｓｔｗａｖｅｆｒｏｍｔｈｅｓｕｎｃａｎｃｏｍｐｒｅｓｓｔｈｅｍ… 相似文献
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利用一维自洽的时变极区电离层模型,研究极隙区极光粒子沉降对极区电离层F层电子密度影响的时变过程。假设一维时变电离层模型描述的磁流管中F层等离子体在对流作用下经过极隙区,随对流路径的不同,磁流管在极隙区经历的时间不同,以此考察极光粒子沉降作用下电离层随时间的演化过程。数值计算结果表明,当磁流管在极隙区停留的时间足够长,F层电子密度能显著增大。然而在磁流管经历极隙区实际时间较短的情况下,极隙区极光粒子沉降对F层电子密度的影响并不大。本文还给出了统计对流模型作用下磁流管在经历极隙区时,有沉降粒子作用和没有沉降粒子作用两种情况下,F层等离子体的时间变化过程的差异。 相似文献
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午后极光强度与行星际磁场的相关 总被引：2，自引：0，他引：2
利用1997年和199年南极中山站多通道扫描光度计的地面观测数据和WIND卫星在弓激波上游对行星际磁场(IMF)的观测数据,对午后高纬极光强度与IMF各分量、以及时钟角之间的相关进行了定量研究. 统计表明,630nm的强度Ir随IMF Bx的增大而减小,其线性相关系数为-0.3;而557.7nm的变化趋势与此相反,其相关系数要低得多. 630nm的强度随IMF By的变化曲线为一"V"形结构,其谷底在By=-3nT附近;557.7nm的强度也有相似的变化趋势,其谷底的位置在By=-2nT附近. 极光强度随IMF Bz的变化曲线为一倒着的"Z"字形结构. 630nm的强度随IMF的模B的增大而增强,其线性相关系数达到0.9,而557.7nm与B之间的相关性要差得多. 极光强度随IMF时钟角的变化曲线为一倒"V"结构,其反转点在θ=130°附近. 相似文献
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Using the ground observation data at Zhongshan Station of Antarctica during July 13 to 17, 2000, the intense absorption events associated with the activities of the solar active region R9077 are analyzed. It was shown that an intense polar cap absorption event lasted more than 3 days, which was caused by the solar proton event associated with the X5/3B major flare at 1024 UT on July 13. The polar cap event started at about 1040 UT on July 14, and lasted to about 1940 UT on July 17, with a typical day night variation. At the same time, the intense solar activities extremely disturbed the magnetosphere, therefore aurora substorms occurred frequently. The energetic particle precipitation from the magnetosphere caused several absorption spikes superposing on the background of polar cap absorption. One distinct event is the absorption enhancement that started at about 0300 UT on July 15, reached its peak of 26 dB at about 0645 UT and recovered at about 1110 UT on the same day, which was the strongest absorption event observed at Zhongshan Station since the imaging riometer installed in February, 1997. Another outstanding absorption spike with pulsation occurred at about 1753 UT on 14th, its peak reached to 6 dB. 相似文献
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Intensity variations of the postnoon auroral bright spots observed at Zhongshan Station, Antarctica on August 8, 1999 
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下载免费PDF全文 In this paper we use the high speed multi channel meridian scanning photometer data and all sky TV camera images to analyze the intensity variations of the postnoon auroral bright sports of 557.7 nm and 630.0 nm emissions. Several results can be obtained from this paper. (1) Bright spots are rather transient features lasting typically for only a few minutes. (2) The intensity of the postnoon bright spots of 557.7 nm emissions can surpass 11 kR. The occurrence of the bright spots seems rather frequent. (3) The ratios of I(427.8)/I(630.0) and I(427.8)/I(557.7) during the bright spots occurring time show a positive peak and negative peak respectively. It qualitatively indicates that the average precipitating electron energies along the meridianal scan above Zhongshan Station increased as the bright spot appeared. And the intensification of the spot mainly was caused by the increasing of high energy (3 10 keV) flux. (4) Usually the bright spots are accompanied with the magnetic pulsation and the occurrence of multi band arcs. 相似文献
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Two induction magnetometers have been installed at Chinese Zhongshan Station and Australia Davis Station, Antarctica respectively. We adopt the cross spectral analysis technique to analyze the data of the two induction magnetometers, in June, September, December 1996 and March 1997, and to investigate Pc5 frequency range pulsation (150 600 s) occurrence and propagation in cusp latitude. The results are summarized as follows: At Zhongshan Davis Station, the magnetic pulsations in Pc5 frequency band can occurs over a wide time, but more frequently at pre local magnetic noon and pre local magnetic midnight. The Pc5 pulsations have no significant seasonal variation in the amplitude, occurrence and propagation. The amplitude has a small peak at pre local magnetic noon and large value sometimes at pre local magnetic midnight. In daytime, the Pc5 pulsations propagate westward in morning and eastward in afternoon, and reversal at local magnetic noon. In nighttime, the Pc5 pulsations propagate westward before 20:00 MLT and eastward after 20:00 MLT. Near dusk time, the Pc5 pulsations propagate irregularly. These characteristics indicate that the Pc5 pulsations have different source at different local magnetic time. 相似文献
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