Coronal Mass Ejections from Sunspot and non-Sunspot Regions

TL;DR

This paper investigates the origins and characteristics of coronal mass ejections (CMEs) from both sunspot and non-sunspot regions, analyzing their associations with solar activity and magnetic regions.

Contribution

It provides a comparative analysis of CMEs from sunspot and non-sunspot regions, highlighting differences in their origins and correlations with solar activity.

Findings

Halo CMEs often originate from sunspot regions.

CME occurrence rates correlate with sunspot numbers, especially during rise and decline phases.

High-latitude CMEs from polar crown filaments are less related to sunspots.

Abstract

Coronal mass ejections (CMEs) originate from closed magnetic field regions on the Sun, which are active regions and quiescent filament regions. The energetic populations such as halo CMEs, CMEs associated with magnetic clouds, geoeffective CMEs, CMEs associated with solar energetic particles and interplanetary type II radio bursts, and shock-driving CMEs have been found to originate from sunspot regions. The CME and flare occurrence rates are found to be correlated with the sunspot number, but the correlations are significantly weaker during the maximum phase compared to the rise and declining phases. We suggest that the weaker correlation results from high-latitude CMEs from the polar crown filament regions that are not related to sunspots.