We study the evolution of a mini-filament eruption in a quiet region at the center of the solar disk and its impact on the ambient atmosphere. We used high-spectral resolution imaging spectroscopy in H$\alpha$ acquired by the echelle spectrograph of the Vacuum Tower Telescope (VTT), Tenerife, Spain, photospheric magnetic field observations from the Helioseismic and Magnetic Imager (HMI), and UV/EUV imaging from the Atmospheric Imaging Assembly (AIA) of the Solar Dynamics Observatory (SDO). The H$\alpha$ line profiles were noise-stripped using Principal Component Analysis (PCA) and then inverted to produce physical and cloud model parameter maps. The minifilament formed between small-scale, opposite-polarity magnetic features through a series of small reconnection events and it erupted within an hour after its appearance in H$\alpha$. Its development and eruption exhibited similarities with large-scale erupting filaments, indicating the action of common mechanisms. Its eruption took place in two phases, namely a slow rise and a fast expansion, and it produced a coronal dimming, before the minifilament disappeared. During its eruption we detected a complicated velocity pattern, indicative of a twisted, thread-like structure. Part of its material returned to the chromosphere producing observable effects on nearby low-lying magnetic structures. Cloud model analysis showed that the minifilament was initially similar to other chromospheric fine structures, in terms of optical depth, source function and Doppler width, but it resembled a large-scale filament on its course to eruption. High spectral resolution observations of the chromosphere can provide a wealth of information regarding the dynamics and properties of minifilaments and their interactions with the surrounding atmosphere.

中文翻译：

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喷发微丝的高分辨率光谱及其对附近色层的影响

我们研究了太阳盘中心安静区域的微型灯丝喷发的演变及其对周围大气的影响。我们使用了西班牙特内里费真空塔望远镜 (VTT) 的阶梯光谱仪、日震和磁成像仪 (HMI) 的光球磁场观测以及 UV/EUV 获得的 H$\alpha$ 中的高光谱分辨率成像光谱来自太阳动力学天文台 (SDO) 大气成像组件 (AIA) 的成像。H$\alpha$ 线轮廓使用主成分分析 (PCA) 进行噪声剥离，然后反转以生成物理和云模型参数图。通过一系列小的重联事件，在小尺度、相反极性的磁特征之间形成了微型细丝，并在它出现在 H$\alpha$ 后的一个小时内喷发。它的发展和喷发表现出与大规模喷发的细丝相似，表明了共同机制的作用。它的喷发经历了缓慢上升和快速膨胀两个阶段，并在微丝消失之前产生了日冕变暗。在它的喷发过程中，我们检测到一个复杂的速度模式，表明它是一种扭曲的线状结构。它的部分材料返回色球层，对附近的低洼磁性结构产生了可观察到的影响。云模型分析表明，该微型丝状体最初在光学深度、源函数和多普勒宽度方面与其他色球精细结构相似，但它在喷发过程中类似于一个大型丝状体。