| 南极中山站电离层的极区特征 |
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| 引用本文： | 沈长寿,资民筠,王劲松,刘顺林,徐寄遥.南极中山站电离层的极区特征[J].地球物理学报,2005,48(1):1-6. |
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| 作者姓名： | 沈长寿 资民筠 王劲松 刘顺林 徐寄遥 |
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| 作者单位： | 北京大学地球与空间科学学院,北京,100871;中国极地研究中心,上海,200129;中国科学院空间天气开放研究实验室,北京,100080 |
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| 基金项目： | 国家自然科学基金项目 (4 0 3 740 5 8)、(4 0 13 40 2 0 )、(4 0 2 2 5 0 11)，国家重点基础研究专项基金项目 (G2 0 0 0 0 7840 7)联合资助 |
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| 摘 要： | 本文利用1996年的电离层数字测高仪DPS-4所测的f0F2、f0E以及美国NOAA和DMSP卫星观测估算的半球功率指数和午夜极光区赤道侧边界纬度等资料，考察中山站电离层的极区特征。结果表明，在太阳和地磁宁静环境下，冬季极夜磁正午中山站处于极隙区中心时，电离层内的电离密度达全天的最大值；上、下午各有数小时间隔位极光带内时，高能粒子的电离作用也很重要；夜间进入极差区后，电子密度则很低。夏季极昼时，太阳EUV辐射的电离效应使电离层电离密度比冬季值大许多，而且，日变化的最大值时间也提前了1~2h，强磁扰时，极隙区和极光带均向低纬侧移动；中山站上空的电子密度会大幅度下降。在中等扰动环境下情况要加复杂：磁正午前后极隙区内软粒子沉降的电离强度有所减小，而上、下午极光区的高能粒子电离则有较大增加。
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| 关 键 词： | 电离层f0F2和f0E 极隙区软粒子沉降 极光区粒子电离 太阳EUV辐射 |
| 文章编号： | 0001-5733(2005)01-0001-06 |
| 收稿时间： | 2003-09-04 |
| 修稿时间： | 2003年9月4日 |
FEATURES OF THE POLAR IONOSPHERE AT ZHONGSHAN STATION |
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| SHEN Chang-Shou,ZI Min-Yun,WANG Jin-Song,LIU Shun-Lin,XU Ji-Yao School of Earth and Space Science,Peking University,Beijing ,China Polar Research Center of China,Shanghai ,China Laboratory of Space Weather,Chinese Academy of Sciences,Beijing ,China.FEATURES OF THE POLAR IONOSPHERE AT ZHONGSHAN STATION[J].Chinese Journal of Geophysics,2005,48(1):1-6. |
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| Authors: | SHEN Chang-Shou ZI Min-Yun WANG Jin-Song LIU Shun-Lin XU Ji-Yao School of Earth and Space Science Peking University Beijing China Polar Research Center of China Shanghai China Laboratory of Space Weather Chinese Academy of Sciences Beijing China |
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| Institution: | 1.School of Earth and space Science, Peking University Beijing 100871, China 2 Polar Research Center of China, Shanghai 200129, China 3 Laboratory of Space Weather, Chinese Academy of Science, Beijing 100080, China |
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| Abstract: | We investigate the features of the polar ionosphere over the Zhongshan station in Antarctic using the data of the ionospheric critical frequencies, f oF 2 and f oE, observed by a Digisonde Portable Sounder(DPS-4) at Zhongshan station of Antarctica in 1996, the hemispheric power index and the midnight equatorward boundary of the aurora estimated by the observation of American NOAA and DMSP satellites. The results show that under a quiet environment of the solar activity and geomagnetic variation at the winter polar night, when the station lies in the center of the polar cleft at magnetic noon, the ionization density of the ionosphere attained to a maximum of the diurnal variation. During several hours before noon and afternoon, the ionized effect of the auroral energy particles is also important. At night the electron density is very low when the station situates at the polar cap area. During the summer polar daylight, the ionized effect of the solar EUV radiation makes the ionospheric electron density much larger and the peak time of the diurnal variation of f oF 2 1-2 hr earlier than that in winter. During a strong geomagnetic disturbance, the locations of both the cleft and aurora move to lower latitudes, and the ionospheric electron density over the Zhongshan station decreases significantly. For a moderate disturbed situation, things become more complex: The strength of ionization caused by soft particles in the cleft around the magnetic noon decreases somewhat, while ionization caused by higher energy particles in the aurora area increases a lot before noon and afternoon. |
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| Keywords: | Ionospheric f oF 2 and f oE Soft particle in the cleft Particle ionization in the aurora Solar EUV radiation |
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