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arXiv 2201.06817astro-ph.SR
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平流层太阳爆发中磁通量绳的建立

Buildup of the Magnetic Flux Ropes in Homologous Solar Eruptions

Rui Wang, Ying D. Liu, Shangbin Yang, Huidong Hu

备注：
Accepted for publication in ApJ. 31 pages, 12 figures
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摘要：

同源日冕物质抛射（CME）是一种有趣的现象，通过比较同源物理条件下的多个CME，有可能研究CME的形成。AR 11283在2011年9月4日出现双极时已经在太阳表面存在了几天。它的正极性与先前存在的属于另一个双极的负极性碰撞，沿着碰撞极性之间的极性反转线（PIL）产生周期性的太阳活动，即所谓的碰撞PIL（cPIL）。结果表明，大量的能量和螺旋度以磁通量绳（MFR）的形式积累，并伴随着周期性的释放和积累过程。这些MFRs是沿着cPIL建立的。采用通量亏损方法，表明由于Chintzoglou等人提出的碰撞剪切情景，沿cPIL发生磁抵消。抵消通量的总量为$\sim$ 0.7 $\times$ 10 $^{21}$ Mx，在30 $^\circ$太阳中心距离的置信区域内，不确定度为$\sim$ 13.2 $\%$。抵消的通量相当于双极磁性区域的总无符号通量的24 $\%$。结果表明，碰撞后cPIL附近的磁场发生了很大的剪切，平均剪切角大于70 $^\circ$。MFRs扭曲核的快速膨胀和持续的喷发活动都是由碰撞剪切过程驱动的。这些结果对于更好地理解与同源太阳爆发相关的MFR的建立过程具有重要意义。

英文摘要：

Homologous coronal mass ejections (CMEs) are an interesting phenomenon, and it is possible to investigate the formation of CMEs by comparing multi-CMEs under a homologous physical condition. AR 11283 had been present on the solar surface for several days when a bipole emerged on 2011 September 4. Its positive polarity collided with the pre-existing negative polarity belonging to a different bipole, producing recurrent solar activities along the polarity inversion line (PIL) between the colliding polarities, namely the so-called collisional PIL (cPIL). Our results show that a large amount of energy and helicity were built up in the form of magnetic flux ropes (MFRs), with recurrent release and accumulation processes. These MFRs were built up along the cPIL. A flux deficit method is adopted and shows that magnetic cancellation happens along the cPIL due to the collisional shearing scenario proposed by Chintzoglou et al. The total amount of canceled flux was $\sim$0.7$\times$10$^{21}$ Mx with an uncertainty of $\sim$13.2$\%$ within the confidence region of the 30$^\circ$ sun-center distance. The canceled flux amounts to 24$\%$ of the total unsigned flux of the bipolar magnetic region. The results show that the magnetic fields beside the cPIL are very sheared, and the average shear angle is above 70$^\circ$ after the collision. The fast expansion of the twist kernels of the MFRs and the continuous eruptive activities are both driven by the collisional shearing process. These results are important for better understanding the buildup process of the MFRs associated with homologous solar eruptions.

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