"Dandelion" Filament Eruption and Coronal Waves Associated with a Solar Flare on 2011 February 16

TL;DR

This study investigates a filament eruption and associated coronal waves during a 2011 solar flare, using multi-wavelength high-resolution observations to analyze the dynamics and interactions of coronal disturbances.

Contribution

It provides a detailed three-dimensional velocity analysis of a filament eruption and confirms the activation of distant filaments by EUV coronal waves, enhancing understanding of solar flare-associated disturbances.

Findings

Filament eruption had a 'dandelion' shape with measurable velocity.

Winking filaments far from the flare site were activated by EUV coronal waves.

No Moreton wave was observed despite coronal disturbances.

Abstract

Coronal disturbances associated with solar flares, such as H$\alpha$ Moreton waves, X-ray waves, and extreme ultraviolet (EUV) coronal waves are discussed herein in relation to magnetohydrodynamics fast-mode waves or shocks in the corona. To understand the mechanism of coronal disturbances, full-disk solar observations with high spatial and temporal resolution over multiple wavelengths are of crucial importance. We observed a filament eruption, whose shape is like a "dandelion", associated with the M1.6 flare that occurred on 2011 February 16 in the H$\alpha$ images taken by the Flare Monitoring Telescope at Ica University, Peru. We derive the three-dimensional velocity field of the erupting filament. We also identify winking filaments that are located far from the flare site in the H$\alpha$ images, whereas no Moreton wave is observed. By comparing the temporal evolution of the winking filaments with those of the coronal wave seen in the extreme ultraviolet images data taken by the Atmospheric Imaging Assembly on board the {\it Solar Dynamics Observatory} and by the Extreme Ultraviolet Imager on board the {\it Solar Terrestrial Relations Observatory-Ahead}, we confirm that the winking filaments were activated by the EUV coronal wave.