论文标题
新兴太阳活动区域的磁性螺旋和能量及其杂散
Magnetic helicity and energy of emerging solar active regions and their erruptivity
论文作者
论文摘要
目标。我们研究了磁性螺旋和磁能的积累在新兴太阳活性区域（ARS）中产生的冠状质量弹出（CME）中的作用。方法。使用太阳能动力学观测站上的Helioseismic和磁成像仪获得的矢量磁场数据，我们计算了磁性螺旋和磁能喷射速率以及从磁通磁力出现的开始时间到达45 $^{\ WEST的45 $^{\ WEST（W45）的52个新兴AR的累积预算。结果。其中七个AR产生了CME，而45个AR没有。从统计意义上讲，与非爆发的磁性螺旋性和能量预算相比，爆发性的AR在磁通出现阶段的开始时间和末端（i）开始，而在通量出现阶段结束时，（ii）AR产生其第一个CME或交叉W45时，首先发生W45时。我们发现磁性螺旋和能量阈值$ 9 \ times 10^{41} $ mx $^2 $和$ 2 \ times 10^{32} $ erg，如果交叉，ARS可能会爆发。在一种情况下，当AR在其出现阶段早期爆发，而在六种情况下，非爆发的AR爆发，而在六种情况下，非爆发的AR爆发AR被违反了非爆发AR的隔离，而非爆发的AR则违反了隔离。衰减指数计算可能表明这些AR没有爆发，因为上覆的磁场提供了比喷发ARS更强或更扩展的限制。结论。我们的结果表明，新兴的AR在积累了磁性螺旋和能量的重要预算时倾向于产生CME。任何对其喷发潜力的研究都应将磁性螺旋性与磁能相等的基础。
Aims. We investigate the role of the accumulation of both magnetic helicity and magnetic energy in the generation of coronal mass ejections (CMEs) from emerging solar active regions (ARs). Methods. Using vector magnetic field data obtained by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, we calculate the magnetic helicity and magnetic energy injection rates as well as the resulting accumulated budgets in 52 emerging ARs from the start time of magnetic flux emergence until they reach heliographic longitude of 45$^{\circ}$ West (W45). Results. Seven of the ARs produced CMEs while 45 did not. In a statistical sense, the eruptive ARs accumulate larger budgets of both magnetic helicity and energy than the noneruptive ones over intervals that start from flux emergence start time and end (i) at the end of flux emergence phase, and (ii) when the AR produces its first CME or crosses W45, whichever happens first. We found magnetic helicity and energy thresholds of $9 \times 10^{41}$ Mx$^2$ and $2 \times 10^{32}$ erg, respectively, which, if crossed, ARs are likely to erupt. The segregation, in terms of accumulated magnetic helicity and energy budgets, of the eruptive ARs from the noneruptive ones is violated in one case when an AR erupts early in its emergence phase and in six cases with noneruptive ARs exhibiting large magnetic helicity and energy budgets. Decay index calculations may indicate that these ARs did not erupt because the overlying magnetic field provided stronger or more extended confinement than in eruptive ARs. Conclusions. Our results indicate that emerging ARs tend to produce CMEs when they accumulate significant budgets of both magnetic helicity and energy. Any study of their eruptive potential should place magnetic helicity on equal footing with magnetic energy.
