论文标题
两种类型的约束太阳耀斑的动态特性和磁性非电位性
Dynamic Property and Magnetic Nonpotentiality of Two Types of Confined Solar Flares
论文作者
论文摘要
我们在2010年$ - $ 2019中分析了152个大型燃烧耀斑（从磁盘中心$ \ geq $ m1.0和$ \ leq $ 445^{\ circ} $），并根据Li等人的工作中的标准将它们分为两种类型。 （2019）。 “ I型”耀斑的特征是耀斑环和缎带的滑动运动以及耀斑环的稳定细丝。 “ II型”耀斑与细丝的失败喷发有关，可以通过经典的2D耀斑模型来解释。总共59个耀斑是“ I型”耀斑（约40 \％），而93个事件是“ II型”耀斑（约60 \％）。积极区域（ARS）的总未签名磁通量（$φ$$ _ \ MATHRM {AR} $）的分布存在显着差异，该区域（ARS）产生了两种类型的密闭耀斑，具有“ I型I型”的限制弹力，其ARS具有$ $ $ $ $ $ $ $ $ $ _ {ar} $ ant type ii type ii”。我们在耀斑发作之前计算出AR核心内的平均剪切角$ψ$$ _ \ MATHRM {HFED} $，并发现“ I型”耀斑的耀斑比“ II型”事件略小。相对非电位参数$ψ$$ _ \ mathrm {hfed} $/$φ$$ _ \ mathrm {ar} $在区分两种类型的耀斑方面具有最佳性能。大约73％的“ I型”约束耀斑具有$ψ$$ _ \ mathrm {hfed} $/$/$/$/$φ$$ $ψ$$ _ \ mathrm {hfed} $/$ $/$φ$$ _ \ mathrm {ar} $$ \ geq $ 1.0 $ \ times $$ $$ 10^{ - 21} $ mx $ mx $^{ - 1} $。我们建议“ I型”限制耀斑无法通过2D/3D中的标准耀斑模型来解释，并且复杂磁系统内的多个滑动磁重连接的发生可能会导致观察到的耀斑。
We analyze 152 large confined flares (GOES class $\geq$M1.0 and $\leq$$45^{\circ}$ from disk center) during 2010$-$2019, and classify them into two types according to the criterion taken from the work of Li et al. (2019). "Type I" flares are characterized by slipping motions of flare loops and ribbons and a stable filament underlying the flare loops. "Type II" flares are associated with the failed eruptions of the filaments, which can be explained by the classical 2D flare model. A total of 59 flares are "Type I" flares (about 40\%) and 93 events are "Type II" flares (about 60\%). There are significant differences in distributions of the total unsigned magnetic flux ($Φ$$_\mathrm{AR}$) of active regions (ARs) producing the two types of confined flares, with "Type I" confined flares from ARs with a larger $Φ$$_{AR}$ than "Type II". We calculate the mean shear angle $Ψ$$_\mathrm{HFED}$ within the core of an AR prior to the flare onset, and find that it is slightly smaller for "Type I" flares than that for "Type II" events. The relative non-potentiality parameter $Ψ$$_\mathrm{HFED}$/$Φ$$_\mathrm{AR}$ has the best performance in distinguishing the two types of flares. About 73\% of "Type I" confined flares have $Ψ$$_\mathrm{HFED}$/$Φ$$_\mathrm{AR}$$<$1.0$\times$$10^{-21}$ degree Mx$^{-1}$, and about 66\% of "Type II" confined events have $Ψ$$_\mathrm{HFED}$/$Φ$$_\mathrm{AR}$$\geq$1.0$\times$$10^{-21}$ degree Mx$^{-1}$. We suggest that "Type I" confined flares cannot be explained by the standard flare model in 2D/3D, and the occurrence of multiple slipping magnetic reconnections within the complex magnetic systems probably leads to the observed flare.
