High resolution observations of sympathetic eruptions by NVST

TL;DR

This study presents high-resolution observations of two sympathetic filament eruptions on the Sun, revealing their dynamics, failed nature, and underlying magnetic mechanisms using NVST and SDO data.

Contribution

It provides detailed imaging and magnetic modeling insights into the triggers and evolution of sympathetic filament eruptions.

Findings

Both eruptions were failed, with filaments merging into a larger quiescent filament.

Kink instability likely triggered the left filament eruption.

Magnetic reconnection at an X-point contributed to the right filament eruption.

Abstract

We investigate two sympathetic filament eruptions observed by the New Vacuum Solar Telescope (NVST) on 2015 October 15. The full picture of the eruptions is obtained from the corresponding SDO/AIA observations. The two filaments start from active region NOAA 12434 in the north and end in one large quiescent filament channel in the south. The left filament erupts firstly, followed by the right filament eruption about 10 minutes later. Clear twist structure and rotating motion are observed in both filaments during the eruption. Both eruptions are failed, since the filaments firstly rise up, then flow towards the south and merge into the southern large quiescent filament. We also observe repeating activations of mini filaments below the right filament after its eruption. Using magnetic field models constructed based on SDO/HMI magnetograms by flux rope insertion method, we find that the left filament eruption is likely to be triggered by kink instability, while weakening of overlying magnetic fields due to magnetic reconnection at an X-point between the two filament systems might play an important role in the onset of the right filament eruption.