High-resolution spectroscopy of an erupting minifilament and its impact on the nearby chromosphere

TL;DR

This study uses high-resolution spectroscopic imaging to analyze the eruption of a solar minifilament, revealing its formation, eruption phases, and impact on the surrounding chromosphere, with implications for understanding solar filament dynamics.

Contribution

It provides detailed spectroscopic analysis of a minifilament eruption, highlighting similarities with larger filaments and demonstrating the effectiveness of PCA-based line profile inversion.

Findings

Minifilament formed via small reconnection events between opposite-polarity magnetic features.

Eruption involved slow rise and fast expansion phases, producing coronal dimming.

Eruption caused complex velocity patterns and material fallback affecting nearby magnetic structures.

Abstract

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.