| 午后极光强度与行星际磁场的相关 |
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| 引用本文： | 胡红桥,刘瑞源,杨惠根,王敬芳,N.Sato,M.Kikuchi,李升贵.午后极光强度与行星际磁场的相关[J].地球物理学报,2002,45(4):445-452. |
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| 作者姓名： | 胡红桥 刘瑞源 杨惠根 王敬芳 N.Sato M.Kikuchi 李升贵 |
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| 作者单位： | 1. 中国极地研究所,上海,200129;
2. 武汉大学光电信息学院,武汉,430072;
3. National Institute of Polar Research, Tokyo 173-8515 |
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| 基金项目： | 国家自然科学基金项目 ( 49634 160 ,4 0 10 4 0 0 9,4 0 0 74 38),国家海洋局青年科学基金项目 ( 2 0 0 0 90 3) |
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| 摘 要： | 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.
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| 关 键 词： | 南极 中山站 午后极光 极光强度 扫描光度计 行星际磁场. |
| 文章编号： | 0001-5733(2002)04-0445-08 |
| 收稿时间： | 2001-10-26 |
DEPENDENCE OF THE POSTNOON AURORAL INTENSITY UPON THE IMF |
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| HU HONG-QIAO LIU RUI YUAN YANG HUI GEN WANG JING FANG N.SATO M. KIKUCHI LI SHENG GUI Polar Research Institute of China,Shanghai ,China.DEPENDENCE OF THE POSTNOON AURORAL INTENSITY UPON THE IMF[J].Chinese Journal of Geophysics,2002,45(4):445-452. |
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| Authors: | HU HONG-QIAO LIU RUI YUAN YANG HUI GEN WANG JING FANG NSATO M KIKUCHI LI SHENG GUI Polar Research Institute of China Shanghai China |
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| Institution: | 1. Polar Research Institute of China, Shanghai 200129, China;
2. Department of Radio Science and Technology, Wuhan University, Wuhan 430072, China;
3. National Institute of Polar Research, Tokyo 173 -8515, Japan |
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| Abstract: | Based on auroral observations of a multi channels scanning photometer at Zhongshan Station, Antarctica and interplanetary magnetic field （IMF） data obtained by WIND Satellite at the upstream of the bow shock in 1997 and 1998, the dependence of the high latitude postnoon auroral intensity upon the IMF components and clock angle are studied. It is shown that the 630nm intensity depends on the IMF B x more directly than the 557.7nm does. The 630nm intensity decreases as IMF B x increasing with a correlation coefficient of -0.83, while the 557.7nm intensity is less dependent on IMF B x . The auroral intensity of both 630nm and 557.7nm varies with the IMF B y as a "V" shape, having a minimum at B y =-3nT; while it varies with B z as a lain "Z" shape, having two turning points at B z =-3nT and B z =2nT. The correlation coefficient between the 630nm intensity and the IMF total intensity B is 0.89, while the correlation between the 557.7nm intensity and the IMF B seems not so good. The auroral intensity varies with the IMF clock angle as a invrse "V" structure which turns at θ =130°. |
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| Keywords: | Antarctica Zhongshan Station Postnoon aurora Auroral intensity Scanning photometer IMF |
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