3D MHD Simulation Study of Solar Fares as Derived by the Satellite Yohkoh

在X射线卫星Yohkoh获得的新的观测结果中，我们得出的关于拱廊扩张的新发现与经典的“一旦打开的双极拱廊模型的重合闸”预测的结果大不相同。在目前的工作中，我们专注于寻找一个新的模型，可以解释这些新的观测结果。通过对Yohkoh观测资料的分析，我们发现：（1）拱形成的暗前结构并不是经典模型中所假设的简单的双极磁拱，而是包含了内腿交叉的双拱结构;（2）暗丝飞走后的某个时刻，我们称之为“脊柱”的结构出现了，这在经典模型中是完全没有预料到的。这是由多条细线组成的，不可能是经典模型中可能解释的重连点的轨迹;（3）在拱状耀斑中，我们发现存在着大的环，将耀斑尖点的顶部连接回B上的光球 ...更多信息 在尖点下方的暗隧道的轴附近有一个明亮的结构。这些在经典模型中没有对应的模型。相反，这些发现正是内田提出的模型所能解释的。因此，我们恢复了内田先前提出的“四源模型”，但由于当时缺乏足够好的观测来确认其日冕特征，因此没有成为主流。我们已经开发了一个时间依赖的模拟计划，并寻求解决方案的平衡解决方案。在1996年，我们得出了一个结论，我们一直在发展的四源模型给出了大部分的观察到的行为，如果我们开始从一个压缩态的纵向磁场在中性片在日冕中心的极性反转线以上的动态模拟。这种构型可以以磁应力的形式储存磁能，当一些触发螺旋度注入暗丝部分并将其从中性片中挤出时，它可以释放磁能。储存在整个区域的应力能可以通过重联释放，然后允许重联发生在中性点。这个模型很好地解释了上述观察到的事实，我们开始报道它。减

Among the new observational findings obtained by the Xray Satellite Yohkoh, the new findings we derived about arcade flarings turn out to be quite different from what the classical "reclosing of once opened-up bipolar arcade model" predicted. In the present work, we concentrate on seeking a new model that can explain these new observational findings. What we have found by the analyses of the Yohkoh data were, (1) faint pre-event structure of arcade formation is not a simple bipolar magnetic arcade as assumed in the classical model, but dual arcades side by side with inner legs crossing is invorved, (2) what we call a "spine" comes up rising sometime after the dark filament flies away, quite unexpected in the classical model. This is consisted of multiple thin threads, and can not be the locus of reconnecting points as may be explained in the classical model, and (3) in arcade flares, we found that there exist large loops connecting the top of the flare cusp back to the photosphere on b … More oth sides, and there is a bright structure near the axis of the dark tunnel below the cusp. These have no model counterpart in the classical model. Those findings, in contrast, are exactly what can be explained in the model proposed by Uchida. We, therefore, revived the "Quadruple Source Model" that was previously proposed by Uchida, but did not become the main stream due to the lack of good enough observation to confirm its coronal characteristic features that time. We have developed the equiliblium solution into a time-dependent simulation scheme, and seek solutions. In 1996, we reached a conclusion that the quadruple source model we have been developing give most of the observed behavior if we start the dynamic simulation from a squeezed state with longitudinal magnetic field in the neutral sheet in the corona above the central polarity-reversal line. The configuration can store magnetic energy in the form of magnetic stress, and can release it when some triggering helicity is injected into the dark filament part and squeeze it out from the neutral sheet. The stress energy stored in the entire region can be released through reconnection then allowed the reconnection to occur at the neutral point. This model explain the above-mentioned observed facts pretty well, and we start reporting about it. Less