High-resolution Observation of Mini-Filament Eruptions Near Coronal Hole Boundary and Their Response in Solar Corona

TL;DR

This study uses high-resolution solar observations to analyze mini-filament eruptions near coronal hole boundaries, revealing their role in coronal dynamics, mass transfer, and magnetic flux contributions to the solar corona and wind.

Contribution

It provides the first detailed analysis of small-scale mini-filament eruptions and their impact on coronal activity and solar wind, using high-resolution multi-wavelength data.

Findings

Mini-filament eruptions are linked to localized brightenings and coronal ejections.

Larger eruptions correlate with EUV emissions and magnetic flux cancellation.

Mini-filaments significantly contribute to mass and magnetic flux transfer in the corona.

Abstract

We investigated mini-filament (MF) eruptions near coronal hole (CH) boundaries to explore their role in coronal dynamics and their potential contributions to the solar wind. Using high-resolution H$\alpha$ images from the 1.6m Goode Solar Telescope at Big Bear Solar Observatory and EUV data from AIA 193 \AA~ from Solar Dynamic Observatory, we analyzed 28 MFE events over 7.5 hours of observation spanning 5 days. Three largest MF eruptions triggered distinct coronal responses: two consecutive MFEs produced a small-scale eruptive coronal ejection, while the other generated a jet-like brightening. Furthermore, the 25 smaller-scale MFEs were associated with localized brightenings in coronal bright points (CBPs). These findings suggest that MFs play a significant role in transferring mass and magnetic flux to the corona, particularly within CH regions. We found certain trend that the size of MFEs is correlated with the EUV emissions. In addition, we observed magnetic flux cancellation associated with MFEs. However, except for a few largest MFEs, quantitative analysis of magnetic field evolution is beyond the capability of the data. These results underscore the importance of MFEs in the dynamic coupling between the chromosphere and corona, highlighting their potential role in shaping heliospheric structures. Although current study covers smallest MFEs ever studied, future higher-cadence, more accurate magnetograms and multi-wavelength observations are essential to fully resolve the fine-scale dynamics of these ubiquitous solar phenomena.