Convection-driven Multiscale Magnetic Fields Determine the Observed Solar Disk Gamma Rays

Abstract The solar disk is a continuous source of GeV–TeV gamma rays. The emission is thought to originate from hadronic Galactic cosmic rays (GCRs) interacting with the gas in the photosphere and uppermost convection zone after being reflected by solar magnetic fields. Despite this general understanding, existing theoretical models have yet to match observational data. At the photosphere and the uppermost convection zone, granular convection drives a multiscale magnetic field, forming a larger-scale filamentary structure while also generating turbulence-scale Alfvén wave turbulence. Here, we demonstrate that the larger-scale filamentary field shapes the overall gamma-ray emission spectrum, and the Alfvén wave turbulence is critical for further suppressing the gamma-ray emission spectrum below ∼100 GeV. For a standard Alfvén wave turbulence level, our model’s predicted spectrum slope from 1 GeV to 1 TeV is in excellent agreement with observations from the Fermi Large Area Telescope and HAWC, an important achievement. The predicted absolute flux is a factor of 2–5 lower than the observed data; we outline future directions to resolve this discrepancy. The key contribution of our work is providing a new theoretical framework for using solar disk gamma-ray observations to probe hadronic GCR transport in the lower solar atmosphere.