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首页> 外文期刊>Earth, planets and space: EPS >Geomagnetic effects of high-density plasma with southward magnetic field in the interplanetary coronal mass ejection observed on May 2-3, 1998
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Geomagnetic effects of high-density plasma with southward magnetic field in the interplanetary coronal mass ejection observed on May 2-3, 1998

机译：1998年5月2-3日观测到的行星际日冕物质抛射中高密度等离子体在南磁场的作用下的地磁效应

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This paper aims to clarify the effect of high-density plasma in interplanetary coronal mass ejection (ICME) observed during the May 2-3, 1998 geomagnetic storm. The examination is performed based on the estimation of Dst index, which is calculated with the observed solar wind parameters of the ICME. The estimated Dst index variation is compared with Dst index variation provided by the World Data Center for Geomagnetism, Kyoto (WDC, Kyoto). From this examination, we find that the trend of the estimated Dst is in good agreement with that of the provided Dst when the thresholds are taken into account for both the solar wind plasma density and the dawn-to-dusk solar wind electric field, as 30 #/cc and 0.49 mV/m, respectively. From the result, we can conclude that the effect of high-density plasma is important on the enhancement of geomagnetic storm as well as the effect of the other solar wind parameters, such as the interplanetary magnetic field (IMF) Bz and solar wind velocity. On the other hand, the solar source of the magnetic field of this ICME is examined. The magnetic field structure of the ICME is examined by fitting the flux rope model to the observed magnetic field and solar wind speed. The results are compared with the magnetic structure of the bases of coronal helmet streamers. From this comparison we can find that the magnetic structure of the interplanetary flux rope is in good agreement with that of the neutral line of the base of coronal helmet streamers. The result suggests that if we look for the causes of geomagnetic storm we should take into account both the plasma structure and the magnetic structure of the base of coronal helmet streamers.
机译：本文旨在阐明在1998年5月2-3日的地磁风暴中观测到的高密度等离子体对行星际冠状物质抛射（ICME）的影响。该检查是基于Dst指数的估算执行的，该估算是根据ICME观测到的太阳风参数计算得出的。将估计的Dst指数变化与京都世界地磁数据中心（WDC，京都）提供的Dst指数变化进行比较。通过此检查，我们发现，当同时考虑到太阳风等离子体密度和黎明至黄昏太阳风电场的阈值时，估计Dst的趋势与提供的Dst的趋势非常吻合。 30＃/ cc和0.49 mV / m。从结果可以得出结论，高密度等离子体的影响对于增强地磁风暴以及其他太阳风参数（如行星际磁场（IMF）Bz和太阳风速）的影响都很重要。另一方面，检查该ICME的磁场的太阳能源。通过将通量绳模型拟合到观测到的磁场和太阳风速来检查ICME的磁场结构。将结果与冠状头盔彩带底座的磁性结构进行了比较。从这个比较中我们可以发现，行星际通量绳索的磁性结构与冠状头盔彩带底座的中性线的磁性结构非常吻合。结果表明，如果我们寻找地磁风暴的原因，则应同时考虑冠状头盔彩带底部的等离子体结构和磁性结构。

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