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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Interplanetary conditions causing intense geomagnetic storms (Dst ≤ ?100 nT) during solar cycle 23 (1996–2006)
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Interplanetary conditions causing intense geomagnetic storms (Dst ≤ ?100 nT) during solar cycle 23 (1996–2006)

机译：星际条件引起强烈地磁风暴在太阳能(Dst≤? 100元)23周期(1996—2006)

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The interplanetary causes of intense geomagnetic storms and their solar dependence occurring during solar cycle 23 (1996–2006) are identified. During this solar cycle, all intense (Dst ≤ ?100 nT) geomagnetic storms are found to occur when the interplanetary magnetic field was southwardly directed (in GSM coordinates) for long durations of time. This implies that the most likely cause of the geomagnetic storms was magnetic reconnection between the southward IMF and magnetopause fields. Out of 90 storm events, none of them occurred during purely northward IMF, purely intense IMF By fields or during purely high speed streams. We have found that the most important interplanetary structures leading to intense southward Bz (and intense magnetic storms) are magnetic clouds which drove fast shocks (sMC) causing 24% of the storms, sheath fields (Sh) also causing 24% of the storms, combined sheath and MC fields (Sh+MC) causing 16% of the storms, and corotating interaction regions (CIRs), causing 13% of the storms. These four interplanetary structures are responsible for three quarters of the intense magnetic storms studied. The other interplanetary structures causing geomagnetic storms were: magnetic clouds that did not drive a shock (nsMC), non magnetic clouds ICMEs, complex structures resulting from the interaction of ICMEs, and structures resulting from the interaction of shocks, heliospheric current sheets and high speed stream Alfvén waves. During the rising phase of the solar cycle, sMC and sheaths are the dominant structure driving intense storms. At solar maximum, sheath fields, followed by Sh+MCs and then by sMC were responsible for most of the storms. During the declining phase, sMC, Sh and CIR fields are the main interplanetary structures leading to intense storms. We have also observed that around 70% of the storms follow the interplanetary criteria of Ey ≥ 5 mV/m for at least 3 h. Around 90% of the storms used in the study followed a less stringent set of criteria: Ey ≥ 3 mV/m for at least 3 h. Finally, we obtain the approximate rate of intense magnetic storms per solar cycle phases: minimum/rising phase 3 storms.year?1, maximum phase 8.5 storms.year1, and declining/minimum phases 6.5 storms.year1.
机译：激烈的星际原因地磁风暴和太阳能产生的依赖在太阳活动周期23(1996 - 2006)进行标识。在这太阳周期,所有紧张(Dst≤100英镑nT)地磁风暴时被发现向南的行星际磁场导演(GSM坐标)很长时间的时间。磁暴的磁性国际货币基金组织和向南之间的重新连接磁字段。发生在纯粹的国际货币基金组织(IMF)向北,纯粹的激烈的国际货币基金组织(IMF)字段或在纯粹高速流。重要的星际结构导致强烈的向南(Bz报道和强烈的磁场风暴)磁云开快冲击(sMC)导致24%的风暴,鞘字段(Sh)也导致24%的风暴,结合鞘和MC字段(Sh + MC)造成16%风暴,共转交互区域(cir),导致13%的风暴。星际结构负责四分之三的强烈磁场风暴研究。引起磁暴是:磁云不开冲击(nsMC),非磁性云icm,造成复杂的结构icm的互动,和结构造成冲击,之间的相互作用日球电流片和高速流阿尔芬波。太阳活动周期,sMC和鞘是占主导地位的结构驱动强烈的风暴。最大,鞘字段,Sh + MCs和紧随其后然后由sMC负责大部分的风暴。CIR字段是主要的星际结构导致强烈的风暴。按照70%左右的风暴星际的标准是≥5 mV / m3 h。大约90%的风暴中使用研究了一套不严格的标准:莎莉≥3 mV / m至少3 h。最后,我们获得近似的强烈的磁性风暴每一个太阳活动周期阶段:最小/上升阶段3storms.year吗?和下降/ 6.5 storms.year1最低阶段。

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