Onset mechanism of solar eruptions
Onset mechanism of solar eruptions
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DOI：
10.1016/j.jastp.2017.08.035
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发表时间：
2017-09
影响因子：
1.9
通讯作者：
S. Inoue;Y. Bamba;K. Kusano
中科院分区：
文献类型：
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作者：
S. Inoue;Y. Bamba;K. Kusano
太阳爆发是太阳系中观测到的能量最大的现象，如耀斑、日冕物质抛射（CME）和日珥/暗条爆发。螺旋扭曲的通量管被广泛认为是太阳爆发的来源和驱动器，并将等离子体带入行星际空间。这些物质最终可能到达磁层，造成地磁场的强烈扰动。因此，了解太阳爆发的开始不仅在太阳物理学框架内而且对空间气象预报都很重要。在本文中，我们报告了新的见解，最近从我们的新研究中获得的太阳爆发的发病机制。我们使用最先进的太阳物理卫星进行观测研究，并使用最新的超级计算机系统进行数值研究。我们指出了光球磁场的两种小磁扰动。这些可以增强预先存在的非潜在磁场中的磁重联，从而产生大通量管，然后驱动喷发。我们进一步证实，这种重新连接是我们最新数据约束模拟中爆发的关键过程。我们报告我们的最新结果和我们的太阳爆发的发病机制的解释。
Solar eruptions are the most energetic phenomena observed in the solar system observed as flares, coronal mass ejections (CMEs) and filament/prominence eruption. The helically twisted flux tube is widely thought to be the source and driver of solar eruptions and to carry the plasma into the interplanetary space. Those may eventually reach the magnetosphere and cause strong disturbances of the geomagnetic field. Therefore, the understanding of the onset of solar eruptions is important not only in the framework of solar physics but also for the space weather forecast. In this paper, we report on new insight into the onset mechanism of solar eruptions recently obtained from our new studies. We perform the studies in terms of the observational approach with state-of-the-art solar physics satellites and the numerical one with the latest super computer system. We specified two types of small magnetic perturbations of the photospheric magnetic field. These can enhance the magnetic reconnection in the pre-existing non-potential magnetic field, which produces a large flux tube and then drives the eruption. We further confirmed that this reconnection is a key process for the eruption in our latest data-constrained simulation. We report our latest results and our interpretation of the onset mechanism of solar eruptions.