A Statistical Study of CME Properties and of the Correlation Between Flares and CMEs over Solar Cycles 23 and 24

TL;DR

This study analyzes CME properties and their correlation with solar flares over solar cycles 23 and 24, revealing differences in CME characteristics and their relationship with flare flux, using data from SOHO/LASCO and GOES.

Contribution

It provides a comprehensive statistical analysis of CME properties and their correlation with flares across two solar cycles, highlighting differences between catalogs and cycle behaviors.

Findings

Higher CME counts during Cycle 24 peak despite weaker solar activity.

Log-linear relationship between flare flux and CME mass.

Differences in CME velocity and acceleration for flare-associated events.

Abstract

We investigated some properties of coronal mass ejections (CMEs), such as speed, acceleration, polar angle, angular width, and mass, using data acquired by the Large Angle Spectrometric Coronagraph (LASCO) onboard the Solar and Heliospheric Observatory (SOHO) from 31 July 1997 to 31 March 2014, i.e. during the Solar Cycles 23 and 24. We used two CME catalogs: one provided by the Coordinated Data Analysis Workshops (CDAW) Data Center and one obtained by the Computer Aided CME Tracking software (CACTus) detection algorithm. For each dataset, we found that the number of CMEs observed during the peak of Cycle 24 was higher than or comparable to the number during Cycle 23, although the photospheric activity during Cycle 24 was weaker than during Cycle 23. Using the CMEs detected by CACTus, we noted that the number of events [N] is of the same order of magnitude during the peaks of the two cycles, but the peak of the CME distribution during Cycle 24 is more extended in time (N >1500 during 2012 and 2013). We ascribe the discrepancy between the CDAW and CACTus results to the observer bias for CME definition in the CDAW catalog. We also used a dataset containing 19,811 flares of C-, M-, and X-class observed by the Geostationary Operational Environmental Satellite (GOES) during the same period. Using both datasets, we studied the relationship between the mass ejected by the CMEs and the flux emitted during the corresponding flares: we found 11,441 flares that were temporally correlated with CMEs for CDAW and 9120 for CACTus. Moreover, we found a log-linear relationship between the flux of the flares integrated from the start to end in the 0.1 - 0.8 nm range and the CME mass.We also found some differences in the mean CMEs velocity and acceleration between the events associated with flares and those that were not.