| 地磁钩扰的全球响应特征研究与初步统计结果 |
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| 引用本文： | 雷柱,邢赞扬,张清和,韩德胜,陈耀,房嘉成,闫晓燊,黄可之,何川.地磁钩扰的全球响应特征研究与初步统计结果[J].地球物理学报,2018,61(2):437-448. |
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| 作者姓名： | 雷柱 邢赞扬 张清和 韩德胜 陈耀 房嘉成 闫晓燊 黄可之 何川 |
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| 作者单位： | 1. 山东大学(威海)空间科学与物理学院 山东大学空间科学研究院 山东省光学天文与日地空间环境重点实验室, 山东威海 264209;2. 中国极地研究中心 国家海洋局极地科学重点实验室, 上海 200136;3. 山东大学(威海)机电与信息工程学院, 山东威海 264209 |
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| 基金项目： | 国家自然基金项目（41604139，41574138），山东省杰出青年基金项目（JQ201412）和电波环境特性及模化技术重点实验室基金项目（JW2016-009）资助. |
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| 摘 要： | 地磁钩扰是太阳耀斑效应的直观表现之一，其研究有助于深入理解太阳爆发对地球空间环境的影响过程，并能为空间天气建模和预报提供科学依据.本文利用山东大学威海地磁台和Intermagnet地磁链与子午工程的地磁观测数据，联合GOES卫星及数字测高仪等的数据，研究了一个由M5.6级太阳耀斑引发的地磁钩扰事件的全球响应特征.研究发现：地磁钩扰特征呈现出南北半球与午前/午后的差异，且地磁响应相对于太阳耀斑存在约3 min的滞后现象，而夜侧无明显扰动；利用位于日侧的50余个地磁台站的数据统计分析后发现地磁钩扰幅度呈现正态分布，且在当地时正午附近达到峰值；利用地磁数据反演出钩扰发生时电离层的电流体系Ss和宁静日电流Sq，并用该电流体系解释了此事件中地磁数据的变化特征.另外，本文初步统计了1996-2015年的地磁钩扰事件数以及相关的太阳耀斑事件数，分析后发现X级耀斑引发地磁钩扰的可能性最大，达42%，由M级耀斑引发的地磁钩扰事件数最多，A、B、C级等小耀斑引发地磁钩扰的可能性很小.
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| 关 键 词： | 地磁钩扰 太阳耀斑效应 全球响应 |
| 收稿时间： | 2017-01-16 |
The global characteristic of a magnetic crochet and some statistic results |
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| LEI Zhu,XING ZanYang,ZHANG QingHe,HAN DeSheng,CHEN Yao,FANG JiaCheng,YAN XiaoShen,HUANG KeZhi,HE Chuan.The global characteristic of a magnetic crochet and some statistic results[J].Chinese Journal of Geophysics,2018,61(2):437-448. |
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| Authors: | LEI Zhu XING ZanYang ZHANG QingHe HAN DeSheng CHEN Yao FANG JiaCheng YAN XiaoShen HUANG KeZhi HE Chuan |
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| Affiliation: | 1. Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Shandong University at Weihia, Institute of Space Sciences, Shandong University, Shandong Weihai 264209, China;2. SOA Key Laboratory for Polar Science, Polar Research Institute of China, Shanghai 200136, China;3. School of Mechanical, Electrical & Information Engineering, Shandong University, Shandong Weihai 264209, China |
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| Abstract: | Geomagnetic crochet is believed to be directly related to solar flares. Relevant studies are important to understand the influence of solar eruptions on near-earth space environment, and to develop space weather forecasting techniques. In this paper, using the data from the geomagnetic station of Shandong University (Weihai), the Intermagnet Geomagnetic chain and the Meridian Space Weather Monitoring Project, the GOES satellite and the digital ionosonde system, we investigate a geomagnetic crochet associated with a M5.6 solar flare. Our conclusions are listed as follows. The characteristics of geomagnetic crochet were different between the northern and southern hemispheres and prenoon/postnoon, and the geomagnetic response had about 3 minutes' delay in comparison to the peak time of the solar flare. Geomagnetic disturbance was not obvious at night. We used the data of more than 50 magnetic stations located in the dayside hemisphere and found that the amplitude of geomagnetic crochet had a normal distribution, with the maximum being near noon. At last, we used geomagnetic data to get the crochet current system Ss during the event and the quiet current system Sq during quiet days. Our statistical study on the geomagnetic crochets and solar flares from 1996 to 2015 shows that the X-class flare is most likely the cause of magnetic crochets, and the possibility is about 42%; most magnetic crochets are caused by M-class flares; smaller flares, like A-, B-, C-class flares are hardly associated with magnetic crochets. |
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| Keywords: | Geomagnetic crochet Solar flare effect Global response |
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