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A two-step scenario for both solar flares and magnetospheric substorms: Short duration energy storage

机译：太阳耀斑和磁层亚暴的两步情景：短期储能

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摘要

The basic observations for magnetic storms and substorms at Earth and for flares at the Sun are reviewed for background. We present a common scenario of double magnetic reconnection for both substorms and flares based on previous interplanetary observations and substorm-triggering results. Central to the scenario is that the first magnetic reconnection phase is the source of energy loading for possible substorms and flares. The energy placed in the magnetotail or magnetosphere/at the sun lasts for only a short duration of time however. The energy gets dissipates away rapidly (in some less dramatic form). This scenario predicts that if the initial reconnection process is sufficiently intense and rapid, concomitant substorms and flares occur soon thereafter. If the energy input is less rapid, there may be lengthy delays for the onset of substorms and flares. If external influences (shocks, etc.) occur during the latter energy buildup, the "trigger" will cause a sudden release of this energy. The model also explains reconnection without subsequent substorms and flares. The model addresses the question why strong triggering events are sometimes ineffective.
机译：回顾了对地球上的磁暴和亚暴以及对太阳的耀斑的基本观测，以作为背景。我们基于先前的行星际观测和亚暴触发结果，提出了一种用于亚暴和耀斑的双磁重联的常见方案。该方案的核心是，第一个磁重连阶段是可能的亚暴雨和耀斑的能量负荷来源。然而，置于磁尾或磁层/太阳的能量仅持续很短的时间。能量迅速消散（以不那么戏剧性的形式）。该场景预测，如果初始重新连接过程足够激烈且迅速，此后不久将发生伴随的亚暴和耀斑。如果能量输入的速度较快，则亚暴雨和耀斑的发作可能会延迟很长时间。如果在后面的能量积累过程中发生外部影响（冲击等），则“触发”将导致该能量的突然释放。该模型还解释了重新连接，而没有随后的亚暴和耀斑。该模型解决了为什么强触发事件有时无效的问题。

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