Study the build-up, initiation and acceleration of 2008 April 26 coronal mass ejection observed by STEREO

TL;DR

This study provides a detailed analysis of the 2008 April 26 coronal mass ejection's evolution, from pre-eruption activities to acceleration, using high-cadence multi-wavelength observations to understand the physical processes involved.

Contribution

It offers a comprehensive, phase-by-phase description of CME evolution, highlighting the role of magnetic reconnection and flux rope formation in eruption initiation.

Findings

EUV jets and filament activities preceded the CME, indicating magnetic reconnection.

Eruption was triggered by inner tether-cutting reconnection, not external breakout.

CME acceleration profile matched the reconnection electric field during impulsive acceleration.

Abstract

In this paper, we analyze the full evolution, from a few days prior to the eruption to the initiation, and the final acceleration and propagation, of the CME that occurred on 2008 April 26 using the unprecedented high cadence and multi-wavelength observations by STEREO. There existed frequent filament activities and EUV jets prior to the CME eruption for a few days. These activities were probably caused by the magnetic reconnection in the lower atmosphere driven by photospheric convergence motions, which were evident in the sequence of magnetogram images from MDI (Michelson Doppler Imager) onboard SOHO. The slow low-layer magnetic reconnection may be responsible for the storage of magnetic free energy in the corona and the formation of a sigmoidal core field or a flux rope leading to the eventual eruption. The occurrence of EUV brightenings in the sigmoidal core field prior to the rise of the flux rope implies that the eruption was triggered by the inner tether-cutting reconnection, but not the external breakout reconnection. During the period of impulsive acceleration, the time profile of the CME acceleration in the inner corona is found to be consistent with the time profile of the reconnection electric field inferred from the footpoint separation and the RHESSI 15-25 keV HXR flux curve of the associated flare. The full evolution of this CME can be described in four distinct phases: the build-up phase, initiation phase, main acceleration phase, and propagation phase. The physical properties and the transition between these phases are discussed, in an attempt to provide a global picture of CME dynamic evolution.