南极中山站宁静日午后极光事件分析

南极中山站宁静日午后极光事件分析 Postnoon Aurora Observed at Zhongshan Station, Antartcica During Quiet Period ——A Case Stuty 胡红桥 1 2 3 4 5 first-author 刘瑞源 1 2 3 4 5 杨惠根 1 2 3 4 5 王敬芳 1 2 3 4 5 K.Makita 1 2 3 4 5 M.Kikuchi 1 2 3 4 5 N.Sato 1 2 3 4 5 武汉大学电子信息学学院,武汉,430072 武汉大学电子信息学学院,武汉,430072 中国极地研究所,上海,200129 中国极地研究所,上海,200129 TakushokuUniversity,Tokyo,193 TakushokuUniversity,Tokyo,193 ,Japan ,Japan NationalInstituteofPolarResearch!Tokyo173,8515 NationalInstituteofPolarResearch!Tokyo173,8515 对１９９７ 年６ 月２ 日１１２７～１７００ ＵＴ，在南极中山站（不变地磁纬度为７４．５Ｓ，ＭＬＴ＝ ＵＴ＋ ２）利用全天空极光摄像机和三波段极光扫描光度计观测到的午后极光进行了分析，发现宁静日午后极光的形态随磁地方时变化．在午后早些时候，辉度较弱的冕状极光出现在中山站的极向侧和日向侧；随后出现的是来自日侧的带状极光，该结构东向传播，赤道向运动；在午后较晚的时候出现的是来自夜侧的带状极光．同时将午后极光与当地地磁观测、ＤＭＳＰ／Ｆ１１ 卫星的粒子观测以及ＷＩＮＤ卫星的ＩＭＦ观测进行了对照分析，认为宁静日午后极光中的分离结构是由来自磁层顶附近的粒子沉降产生的，其变化和运动与地磁Ｈ 分量和ＩＭＦＢｚ 分量的变化相关． It is examined that postnoon aurora observed at Zhongshan station （invariant latitude 74.5S, MLT=UT+2）, Antarctica by all sky TV camera and three wavelength （427.8, 557.7, 630.0 nm） meridian scanning photometer during a quiet period of 1127 1 700 UT, June 2, 1997. It is shown that the morphology of postnoon aurora depends on MLT. At early postnoon fade corona occurs at poleward of Zhongshan station, then equatorward moving band /bands from dayside appears, at last band /bands from nightside appears. Comparing optical aurora with local geomagnetic observation, precipitation particle energy spectra observed by DMSP F11 satellite, and IMF data by WIND satellite has been done. It suggests that the auroral structures occurred during quiet postnoon be caused by particle precipitation from dayside magnetopause, and that their activities and movement be correlated with geomagnetic H component and IMF B zvery well. 南极 中山站 宁静日 午后极光 Antarctica Zhongshan station quiet day postnoon aurora P412.3 国家自然科学基金(61672102);国家极地考察办公室资助 1999-05-01 2021-04-01 5