论文标题
主动区域的新磁参数，以区分大型喷发和狭窄的太阳耀斑
A New Magnetic Parameter of Active Regions Distinguishing Large Eruptive and Confined Solar Flares
论文作者
论文摘要
为了调查太阳能活动区域（ARS）中的磁场如何控制耀斑活性，即是限制或喷发耀斑的发生，我们分析了106个地理作战环境卫星（GOOS）$ \ geq $ \ geq $ m1.0 $ \ geq $ m1.0在2010年期间$ -109 $ 2019 $ 2019。我们计算“燃烧极性反转线”区域内的平均特征扭曲参数$α$$ _ {fpil} $，在高光谱磁性自由能密度的领域内，$α$$ _ \ MATHRM {HFED} $，这两者都提供了AR Core区域非稳态的度量。磁扭转被认为与电流驱动的不稳定性（例如螺旋扭结不稳定性）的驱动力有关。我们还计算出产生耀斑的ARS的总未签名磁通量（$φ$$ _ \ MATHRM {ar} $），其中描述了背景场限制的强度。通过考虑背景磁场的约束效果和AR的磁非电位性，我们提出了一个新的参数$α$/$α$/$φ$$ _ \ MATHRM {AR} $，以衡量与冠状质量驱散（CME）相关的大耀斑的概率。我们发现，在大约90％的爆发耀斑中，$α$ _ \ mathrm {fpil} $/$φ$/$φ （2.2 $ \ times $$ 10^{ - 24} $和3.2 $ \ times $$ 10^{ - 24} $ mm $ $^{ - 1} $ mx $^{ - 1} $），而它们在$ \ sim $ 80 \％的约束flares中的关键值小于关键值。这表明新参数$α$/$φ$$ _ \ MATHRM {ar} $非常能够区分喷发耀斑和约束耀斑。我们的研究表明，在限制背景场的AR核心内磁非电位性的相对度量在很大程度上控制了AR产生喷发耀斑的能力。
With the aim of investigating how the magnetic field in solar active regions (ARs) controls flare activity, i.e., whether a confined or eruptive flare occurs, we analyze 106 flares of Geostationary Operational Environmental Satellite (GOES) class $\geq$M1.0 during 2010$-$2019. We calculate mean characteristic twist parameters $α$$_{FPIL}$ within the "flaring polarity inversion line" region and $α$$_\mathrm{HFED}$ within the area of high photospheric magnetic free energy density, which both provide measures of the nonpotentiality of AR core region. Magnetic twist is thought to be related to the driving force of electric current-driven instabilities, such as the helical kink instability. We also calculate total unsigned magnetic flux ($Φ$$_\mathrm{AR}$) of ARs producing the flare, which describes the strength of the background field confinement. By considering both the constraining effect of background magnetic fields and the magnetic non-potentiality of ARs, we propose a new parameter $α$/$Φ$$_\mathrm{AR}$ to measure the probability for a large flare to be associated with a coronal mass ejection (CME). We find that in about 90\% of eruptive flares, $α$$_\mathrm{FPIL}$/$Φ$$_\mathrm{AR}$ and $α$$_\mathrm{HFED}$/$Φ$$_\mathrm{AR}$ are beyond critical values (2.2$\times$$10^{-24}$ and 3.2$\times$$10^{-24}$ Mm$^{-1}$ Mx$^{-1}$), whereas they are less than critical values in $\sim$ 80\% of confined flares. This indicates that the new parameter $α$/$Φ$$_\mathrm{AR}$ is well able to distinguish eruptive flares from confined flares. Our investigation suggests that the relative measure of magnetic nonpotentiality within the AR core over the restriction of the background field largely controls the capability of ARs to produce eruptive flares.
