极地研究

极地研究 ›› 2013, Vol. 25 ›› Issue (1): 35-44.DOI: 10.3724/SP.J.1084.2013.00035

• 研究论文 • 上一篇    下一篇

不同行星际磁场条件下极向运动极光结构的多手段联合观测

邢赞扬1, 2 杨惠根2 韩德胜2 吴振森1 刘俊明2 胡泽骏2 张清和2 刘勇华2 张北辰2 胡红桥2   

  1.  
    1西安电子科技大学理学院，陕西 西安 710071；
    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
  • 收稿日期:2012-08-29 修回日期:2012-09-06 出版日期:2013-03-30 发布日期:2013-03-30
  • 通讯作者: 邢赞扬
  • 基金资助:

    日侧重联极光的多波段观测和产生机制研究;小尺度极光结构的多尺度并行观测与研究;日侧极光粒子沉降的能谱特征研究;极区电离层对日侧磁重联的响应研究;行星际磁场北向偏转触发亚暴的机制研究

MULTI-INSTRUMENT STUDY OF POLEWARD MOVING AURORAL FORMS DURING DIFFERNET INTERPLANETARY MAGNETIC FIELD CONDITIONS

Xing Zanyang1, 2, Yang Huigen2, Han Desheng2, Wu Zhensen1, Liu Junming2, Hu Zejun2, Zhang Qinghe2, Liu Yonghua2, Zhang Beichen2, Hu Hongqiao2   

  1.  
    1School of Science, Xidian University, Xi’an 710071, China;
    2 SOA Key Laboratory for Polar Science, Polar Research Institute of China, Shanghai 200136, China
  • Received:2012-08-29 Revised:2012-09-06 Online:2013-03-30 Published:2013-03-30
  • Contact: XING Zanyang

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摘要： 本文利用北极黄河站三波段全天空成像仪（ASI）的高分辨率的地面极光观测数据，联合欧洲非相干散射雷达（EISCAT）Svalbard雷达（ESR），超级双子极光雷达网（SuperDARN）雷达等观测，研究了发生在2003年12月22日0900-1010 UT时间段内极区电离层极光和等离子体的变化特征。研究发现在不同行星际磁场（IMF）条件下，黄河站极光ASI均观测到了一系列极向运动极光结构（PMAFs），其特征为极光在赤道向一侧点亮后向高纬扩展。这些PMAFs都伴随有明显的粒子沉降特征，且在IMF北向时该粒子沉降能达到更低的电离层E层区域，而此时这些PMAFs相应位置的高纬电离层出现了一个典型反向对流涡，这是高纬（尾瓣）重联的典型特征之一。这些结果表明北向IMF条件下的这些PMAFs是由高纬重联所产生。在IMF南向时，黄河站观测到的PMAFs可跨越更广的地磁纬度，表明其演化时间亦较长，其相应区域的电离层特征也表明该PMAFs由日侧磁层顶低纬磁重联所产生。

关键词: 极向运动极光结构, 行星际磁场, 磁重联

Abstract: Using high temporal resolution optical data obtained from three-wavelength all-sky imagers at Yellow River Station (YSR) (78.92oN, 11.93oE) in Arctic, together with the EISCAT Svalbard radar (ESR) and SuperDARN HF radars, we investigate the aurora and plasma features in the polar ionosphere under different interplanetary magnetic field (IMF) conditions between 0900 and 1010 UT on 22 December 2003. A series of poleward moving auroral forms (PMAFs) are observed to brighten at the equatorward boundary of the dayside auroral oval and then propagate poleward. Simultaneous optical and ESR observations reveal that all of these PMAFs are clear associated with pulsed plasma precipitations. During northward IMF, the plasma can precipitate lower reaching the ionopheric E-region and there is a reverse convection cell associated with these PMAFs, which is one of the typical signatures in the polar ionosphere of the dayside high-latitude (lobe) reconnection. These results indicate that the PAMFs are attribute to the high-latitude reconnection. During southward IMF, the PAMFs observed at YRS show a larger-latitudinal motion indicating a longer mean lifetime, and the associated ionopheric features indicate that the PMAFs are generated by the dayside magnetopause low-latitude reconnection.

Key words: PMAFs, interplanetary magnetic field, reconnection