2026/01/07 by Gregory D. Fleishman, Ivan Oparin, Gelu M. Nita +3 · 1 voice
Physics and Astronomy · #Dust and Plasma Wave Phenomena #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1038/s41550-025-02754-w
published as Published online: 07 January 2026 · Published in Nature Astronomy; 15 pages; 8 figures
openalex publication_date 2026/01/07 · openalex created_date 2026/01/08 · arxiv published 2026/02/01 · arxiv created 2026/07/28 · openalex updated_date 2026/07/28 · arxiv updated 2026/07/28
Analysis of γ-rays in solar flares has suggested a distinct continuum component dominating at MeV energies, which differs from the well-studied X-ray continuum produced by flare-accelerated electrons with spectra steeply falling with energy. The origin, precise spatial location, and extent of this mysterious MeV component have been unknown up to now. If it is produced by bremsstrahlung, such a γ-ray component requires an unusual population of electrons peaked at a few MeV. Here we report a joint study of this MeV-peaked electron population in the 2017-Sep-10 solar flare with Fermi MeV γ-ray data and EOVSA spatially resolved microwave imaging spectroscopy data. We demonstrate that the microwave spectrum from the MeV-peaked distribution has a distinctly different shape from that produced by the electrons with falling energy spectrum. We inspected microwave maps of the flare and identified an evolving area where the measured microwave spectra matched the theoretically expected one for the MeV-peaked population, thus pinpointing the site where this MeV component resides. The locations are in a coronal volume adjacent to the region where prominent release of magnetic energy and bulk electron acceleration were detected, which implies that transport effects play a key role in forming this population.