Eruptions from coronal bright points: A spectroscopic view by IRIS of a mini-filament eruption, QSL reconnection, and reconnection-driven outflows
Eruptions from coronal bright points: A spectroscopic view by IRIS of a mini-filament eruption, QSL reconnection, and reconnection-driven outflows
复制标题
日冕亮点喷发：IRIS 的迷你丝状喷发、QSL 重新连接和重新连接驱动的流出的光谱视图
DOI：
--
复制
发表时间：
2022
影响因子：
6.5
通讯作者：
Haixia Xie
中科院分区：
文献类型：
--
作者：
M. Madjarska;D. Mackay;K. Galsgaard;T. Wiegelmann;Haixia Xie
上下文我们的研究调查了一个与抵消磁推力有关的迷你电影喷发。喷发起源于一个小规模的环复合体，通常被称为日冕亮点（CBP）。该事件是唯一的记录在成像和光谱数据所采取的界面区成像光谱仪（IRIS）。目标。这项调查旨在更好地了解驱动这些无处不在的小规模喷发的物理过程。方法.我们分析了IRIS光谱和狭缝成像观测以及大气成像组件（AIA）的极紫外通道拍摄的图像和太阳动力学天文台上的日震磁成像仪（HMI）的视线磁场数据。由于观测结果只能表明可能的物理过程，我们还采用了基于HMI磁图时间序列的非线性无力场（NLFFF）松弛方法。这使我们能够进一步研究喷发过程中涉及的磁场结构的演变。结果我们在CBP中艾德了一个强烈的小规模增亮，这是一个微闪烁，记录在从色球到闪烁等离子体的发射中。微型喷发是通过热（CBP环）和冷（迷你薄膜）等离子体的喷射表现出来的，这些等离子体记录在成像和光谱数据中。在微弧之前，在IRIS狭缝钳口1400微弧图像中出现了一个细长的明亮特征，位于极性反转线上方。微弧以IRIS像素尺寸变亮开始，并沿伸长特征沿着双向传播。我们检测到，在光谱和成像IRIS数据和AIA数据，强烈的湍流沿着和边缘的细长功能，我们认为，这些代表重连接出湍流。环绕喷发的MF边缘的细长特征的两个边缘演变成J型形状，形成S形外观。通过计算NLFFF模型不同水平面上的挤压因子Q，在极性反转线附近识别出准分界线层（QSL）艾德。结论. CBP光谱成像研究提供了进一步的证据，证明CBP代表了缩小的活动区域，因此，它们可能对太阳大气的质量和能量平衡做出重大贡献。它们是所有典型活动区特征的来源，包括沿着QSL的磁重联，（小）薄膜喷发，（微）爆发，重联出湍流等QSL重联站点具有与所谓的爆炸事件相同的光谱外观，通过强烈的蓝移和红移发射来识别，从而为关于这种光谱现象的真实性质的一个悬而未决的问题提供了答案。
Context. Our study investigates a mini-filament eruption associated with cancelling magnetic fluxes. The eruption originates from a small-scale loop complex commonly known as a coronal bright point (CBP). The event is uniquely recorded in both the imaging and spectroscopic data taken with the Interface Region Imaging Spectrograph (IRIS). Aims. The investigation aims to gain a better understanding of the physical processes driving these ubiquitous small-scale eruptions. Methods. We analysed IRIS spectroscopic and slit-jaw imaging observations as well as images taken in the extreme-ultraviolet channels of the Atmospheric Imaging Assembly (AIA) and line-of-sight magnetic-field data from the Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory. As the observations can only indicate the possible physical processes at play, we also employed a non-linear force-free field (NLFFF) relaxation approach based on the HMI magnetogram time series. This allowed us to further investigate the evolution of the magnetic-field structures involved in the eruption process. Results. We identified a strong small-scale brightening as a micro-flare in a CBP, recorded in emission from chromospheric to flaring plasmas. The mini-eruption is manifested via the ejection of hot (CBP loops) and cool (mini-filament) plasma recorded in both the imaging and spectroscopic data. The micro-flare is preceded by the appearance of an elongated bright feature in the IRIS slit-jaw 1400Å images, located above the polarity inversion line. The micro-flare starts with an IRIS pixel size brightening and propagates bi-directionally along the elongated feature. We detected, in both the spectral and imaging IRIS data and AIA data, strong flows along and at the edges of the elongated feature; we believe that these represent reconnection outflows. Both edges of the elongated feature that wrap around the edges of the erupting MF evolve into a J-type shape, creating a sigmoid appearance. A quasi-separatrix layer (QSL) is identified in the vicinity of the polarity inversion line by computing the squashing factor, Q , in di ff erent horizontal planes of the NLFFF model. Conclusions. This CBP spectro-imaging study provides further evidence that CBPs represent downscaled active regions and, as such, they may make a significant contribution to the mass and energy balance of the solar atmosphere. They are the sources of all range of typical active-region features, including magnetic reconnection along QSLs, (mini-)filament eruptions, (micro-)flaring, reconnection outflows, etc. The QSL reconnection site has the same spectral appearance as the so-called explosive events identified by strong blue-and red-shifted emission, thus providing an answer to an outstanding question regarding the true nature of this spectral phenomenon.