Quantifying CME effects on plasma parameters and elemental abundance recovery during an M1 flare event with X-ray spectroscopy

¹ Department of Physics, University of Helsinki, PO Box 64 00014 Helsinki, Finland
² Isaware Oy, Dynamicum, Erik Palmenin Aukio 1, 00560 Helsinki, Finland
³ Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany

^★ Corresponding author: saara.takala@helsinki.fi

Received: 3 July 2025
Accepted: 19 October 2025

Abstract

Aims. In this study, we examine the evolution of the plasma parameters, elemental abundances, and X-ray emission source during a long-duration M1-class solar flare and analyze the results in relation to the accompanying coronal mass ejection (CME).

Methods. We used SUNSTORM 1/XFM-CS soft X-ray data to study flare characteristics during an eruption that occurred on the Sun on June 24, 2024, from Active Region 13712. The XFM-CS data were fit with a two-component thermal model using PyXspec. Soft X-ray results were connected with X-ray image reconstructions from SolO/STIX data. The X-ray analysis was complemented with remote-sensing data from STEREO-A/SECCHI and EUVI, SOHO/LASCO, and SDO/AIA to provide a detailed account of the event.

Results. The CME onset corresponds to an increase in X-ray flux, plasma temperature, and emission measure. Prominent X-ray loops are observed in extreme ultraviolet (EUV) after the eruption and remain visible throughout the day. STIX imaging results reveal a large, gradually evolving thermal loop-top emission source. The first ionization potential (FIP) bias does not show signs of recovery even hours after the eruption for any of the fitted elements. The results strongly support the claim that the associated CME delays elemental abundance recovery, providing a connection between flares and CMEs that can be observed and studied with X-rays.