Variations in Abundance Enhancements in Impulsive Solar Energetic-Particle Events and Related CMEs and Flares

TL;DR

This study analyzes how element abundance enhancements in impulsive solar energetic-particle events vary with associated solar phenomena, revealing correlations with flare class, CME properties, and coronal temperature.

Contribution

It introduces a detailed analysis of element abundance variations in impulsive SEP events and their relationship with CME and flare characteristics, using a large dataset of 111 events.

Findings

Steep element enhancements are linked to smaller, cooler, and narrower CME events.

Higher-fluence events show flatter enhancements and are associated with hotter plasma and larger CMEs.

3He/4He enhancements are uncorrelated with heavy-element enhancements but relate to CME and flare properties.

Abstract

We study event-to-event variations in the abundance enhancements of the elements He through Pb for Fe-rich impulsive solar energetic-particle (SEP) events, and their relationship with properties of associated coronal mass ejections (CMEs) and solar flares. Using a least-squares procedure we fit the power-law enhancement of element abundances as a function of their mass-to-charge ratio A/Q to determine both the power and the coronal temperature (which determines Q) in each of 111 impulsive SEP events identified previously. Individual SEP events with the steepest element enhancements, e.g. ~(A/Q)^6, tend to be smaller, lower-fluence events with steeper energy spectra that are associated with B- and C-class X-ray flares, with cooler (~2.5 MK) coronal plasma, and with narrow (<100 deg), slower (<700 km/s) CMEs. On the other hand, higher-fluence SEP events have flatter energy spectra, less-dramatic heavy-element enhancements, e.g. ~(A/Q)^3, and come from somewhat hotter coronal plasma (~3.2 MK) associated with C-, M- and even X-class X-ray flares and with wider CMEs. Enhancements in 3He/4He are uncorrelated with those in heavy elements. However, events with 3He/4He > 0.1 are even more strongly associated with narrow, slow CMEs, with cooler coronal plasma, and with B- and C-class X-ray flares than are other Fe-rich impulsive SEP events with smaller enhancements of 3He.