The observed multi-GeV gamma-ray emission from the solar disk --- sourced by hadronic cosmic rays interacting with gas, and affected by complex magnetic fields --- is not understood. Utilizing an improved analysis of the Fermi-LAT data that includes the first resolved imaging of the disk, we find strong evidence that this emission is produced by two separate mechanisms. Between 2010-2017 (the rise to and fall from solar maximum), the gamma-ray emission is dominated by a polar component. Between 2008-2009 (solar minimum) this component remains present, but the total emission is instead dominated by a new equatorial component with a brighter flux and harder spectrum. Most strikingly, although 6 gamma rays above 100 GeV are observed during the 1.4 years of solar minimum, none are observed during the next 7.8 years. These features, along with a 30-50 GeV spectral dip which will be discussed in a companion paper, were not anticipated by theory. To understand the underlying physics, Fermi and HAWC observations of the imminent Cycle 25 solar minimum are crucial.
@article{arxiv.1803.05436,
title = {Evidence for a New Component of High-Energy Solar Gamma-Ray Production},
author = {Tim Linden and Bei Zhou and John F. Beacom and Annika H. G. Peter and Kenny C. Y. Ng and Qing-Wen Tang},
journal= {arXiv preprint arXiv:1803.05436},
year = {2018}
}
Comments
5 pages, 2 figures. Supplemental Material includes an additional 10 pages, 8 figures. To Be Submitted to Physical Review Letters