A Three-Dimensional Velocity of an Erupting Prominence Prior to a Coronal Mass Ejection

TL;DR

This study provides a comprehensive 3D analysis of a prominence eruption and its associated CME, revealing the dynamics of filament collision, loop expansion, and magnetic interactions during a solar flare event.

Contribution

It introduces a detailed 3D velocity measurement of prominence eruptions using multiwavelength observations, enhancing understanding of CME initiation processes.

Findings

3D velocity field of prominence eruption derived from Hα data

Coronal loop expansion following filament collision observed in EUV

CME growth driven by interactions between expanding loops and magnetic field

Abstract

We present a detailed three-dimensional (3D) view of a prominence eruption, coronal loop expansion, and coronal mass ejections (CMEs) associated with an M4.4 flare that occurred on 2011 March 8 in the active region NOAA 11165. Full-disk H$\alpha$ images of the flare and filament ejection were successfully obtained by the Flare Monitoring Telescope (FMT) following its relocation to Ica University, Peru. Multiwavelength observation around the H$\alpha$ line enabled us to derive the 3D velocity field of the H$\alpha$ prominence eruption. Features in extreme ultraviolet were also obtained by the Atmospheric Imager Assembly onboard the {\it Solar Dynamic Observatory} and the Extreme Ultraviolet Imager on board the {\it Solar Terrestrial Relations Observatory - Ahead} satellite. We found that, following collision of the erupted filament with the coronal magnetic field, some coronal loops began to expand, leading to the growth of a clear CME. We also discuss the succeeding activities of CME driven by multiple interactions between the expanding loops and the surrounding coronal magnetic field.