太阳耀斑中的非定常快速驱动自组织临界性
Non-Stationary Fast-Driven Self-Organized Criticality in Solar Flares
摘要：
最初的自组织临界性概念（Bak et al.~ 1987），应用于太阳耀斑统计（Lu and Hamilton 1991），假设一个缓慢驱动和稳定的耀斑速率，保证时间尺度分离（耀斑持续时间和耀斑间等待时间），它再现了耀斑峰值通量和持续时间的幂律分布，但预测了指数等待时间分布。与这些经典的假设相反，我们观察到：（i）在大多数耀斑中存在多个能量耗散事件，（ii）违反时间尺度分离原则，（iii）快速驱动的非平稳耀斑速率，（iv）等待时间$Δt$服从幂律分布，斜率为$α_{Δt} \approx 2.0$，这是由平均耀斑速率和平均等待时间之间的普遍互易性预测的;以及（v）脉冲，其耗散的磁自由能的上升时间和衰减时间在$12\pm6$分钟的时间尺度上，在长持续时间（$\lapprox 4$小时）耀斑中高达13次。这些结果与日冕的长期能量储存不一致（Rosner和Vaiana 1978），但需要光球-色球层电流注入日冕。
英文摘要：
The original concept of self-organized criticality (Bak et al.~1987), applied to solar flare statistics (Lu and Hamilton 1991), assumed a slow-driven and stationary flaring rate, which warrants time scale separation (between flare durations and inter-flare waiting times), it reproduces power-law distributions for flare peak fluxes and durations, but predicts an exponential waiting time distribution. In contrast to these classical assumptions we observe: (i) multiple energy dissipation episodes during most flares, (ii) violation of the principle of time scale separation, (iii) a fast-driven and non-stationary flaring rate, (iv) a power law distribution for waiting times $Δt$, with a slope of $α_{Δt} \approx 2.0$, as predicted from the universal reciprocality between mean flaring rates and mean waiting times; and (v) pulses with rise times and decay times of the dissipated magnetic free energy on time scales of $12\pm6$ min, up to 13 times in long-duration ($\lapprox 4$ hrs) flares. These results are inconsistent with coronal long-term energy storage (Rosner and Vaiana 1978), but require photospheric-chromospheric current injections into the corona.
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