...
  • 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Solar wind energy input during prolonged, intense northward interplanetary magnetic fields: A new coupling function
【24h】

Solar wind energy input during prolonged, intense northward interplanetary magnetic fields: A new coupling function

机译：太阳能风能输入在长期激烈向北行星际磁场:一个新的耦合函数

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

Sudden energy release (ER) events in the midnight sector auroral zone during intense (B > 10 nT), long-duration (T > 3 h), northward (N = B_z > 0 nT) IMF magnetic clouds (MCs) during solar cycle 23 (SC23) have been examined in detail. The MCs with northward-then-southward (NS) IMFs were analyzed separately from MCs with southwardthen- northward (SN) configurations. It is found that there is a lack of ER/substorms during the N field intervals of NS clouds. In sharp contrast, ER events do occur during the N field portions of SN MCs. From the above two results it is reasonable to conclude that the latter ER events represent residual energy remaining from the preceding S portions of the SN MCs. We derive a new solar wind–magnetosphere coupling function during northward IMFs: E_(NIMF) = a N~-(1/12) V~(7/3) B~(1/2) + βV |Dst_(min)|. The first term on the right-hand side of the equation represents the energy input via “viscous interaction,” and the second term indicates the residual energy stored in the magnetotail. It is empirically found that the magnetotail/magnetosphere/ionosphere can store energy for a maximum of ～4 h before it has dissipated away. This concept is defining one for ER/substorm energy storage. Our scenario indicates that the rate of solar wind energy injection into the magnetotail/ magnetosphere/ionosphere for storage determines the potential form of energy release into the magnetosphere/ionosphere. This may be more important to understand solar wind–magnetosphere coupling than the dissipation mechanism itself (in understanding the form of the release). The concept of short-term energy storage is also applied for the solar case. It is argued that it may be necessary to identify the rate of energy input into solar magnetic loop systems to be able to predict the occurrence of solar flares.
机译：突然的能量释放(ER)事件在午夜在剧烈运动(B部门极光区> 10元),长时间(T > 3 h)、北(N =说是> 0nT)国际货币基金组织(IMF)磁云(MCs)在太阳活动周期23日(SC23)详细检查。northward-then-southward (NS)货币基金分析了MCs southwardthen——分开向北(SN)配置。缺乏在N, ER /亚暴间隔的NS云。ER事件确实发生在N字段的部分SN MCs。可以得出合理的结论,后者ER事件代表剩余残余能量的前S SN MCs的一部分。新的太阳能wind-magnetosphere耦合函数在北方货币基金:E_(带头人)= N ~ - (1/12)V ~ (7/3) B ~(1/2) +βV | Dst_ (min) |。等式的右边代表能量通过粘性相互作用,和输入第二项表示残余能量存储在磁尾。发现磁尾/磁气圈/电离层可以存储能源的最大~ 4 h之前消散了。ER /亚暴能量储存。表明太阳风能量的速度注入的磁尾/磁气圈/电离层存储决定潜在的能量释放到形式磁层、电离层。太阳能wind-magnetosphere重要的理解耦合比耗散机制本身(理解的形式释放)。短期储能也的概念申请太阳能。可能需要确定的能量可以输入太阳磁回路系统预测太阳耀斑的发生。

著录项

相似文献

  • 外文文献
  • 中文文献
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号