A statistical study of the post-impulsive-phase acceleration of flare-associated coronal mass ejections

TL;DR

This study analyzes the post-impulsive-phase acceleration of 247 CMEs associated with solar flares, revealing correlations with flare decay times and solar wind effects, and enhances understanding of CME dynamics.

Contribution

It provides a detailed statistical analysis of CME post-impulsive-phase acceleration and its relation to flare decay times, highlighting the influence of solar wind drag.

Findings

CMEs with long-decay flares tend to have positive post-impulsive acceleration.

CMEs with short-decay flares often show significant deceleration.

Solar wind drag influences deviations from general CME acceleration trends.

Abstract

It is now generally accepted that the impulsive acceleration of a coronal mass ejection (CME) in the inner corona is closely correlated in time with the main energy release of the associated solar flare. In this paper, we examine in detail the post-impulsive-phase acceleration of a CME in the outer corona, which is the phase of evolution immediately following the main impulsive acceleration of the CME; this phase is believed to correspond to the decay phase of the associated flare. This observational study is based on a statistical sample of 247 CMEs that are associated with M- and X-class GOES soft X-ray flares from 1996 to 2006. We find that, from many examples of events, the CMEs associated with flares with long-decay time (or so-called long-duration flares) tend to have positive post-impulsive-phase acceleration, even though some of them have already obtained a high speed at the end of the impulsive acceleration but do not show a deceleration expected from the aerodynamic dragging of the background solar wind. On the other hand, the CMEs associated with flares of short-decay time tend to have significant deceleration. In the scattering plot of all events, there is a weak correlation between CME post-impulsive-phase acceleration and flare decay time. The CMEs deviated from the general trend are mostly slow or weak ones associated with flares of short-decay time; the deviation is caused by the relatively stronger solar wind dragging force for these events. The implications of our results on CME dynamics and CME-flare relations are discussed.