Role of magnetic arcades in explaining the puzzle of the gamma-ray emission from the solar disk
Abstract
The interpretation of gamma-ray emission originating from the solar disk (0.5 in angular size) as due to the interaction of Galactic Cosmic Rays (GCRs) with the solar atmosphere has remained a central challenge in solar physics. After the seminal work by Seckel, Stanev, and Gaisser (SSG91) based on GCRs magnetic mirroring, discrepancies between models and observations persist, indicating the need for a novel approach. The present work focuses on exploring the impact of a closed magnetic field geometry in the low photosphere on the observed gamma-ray flux. We track numerically with the PLUTO code the trajectories of test-particle protons within a static 20 Mm scale height magnetic arcade adjacent to jets. By making use of numerical vertical density profiles we inject particles at distinct chromospheric/photospheric altitudes, mimicking the migration of GCRs from neighboring flux tubes into closed arcades. Remarkably, our model reproduces a flat gamma-ray spectrum below 33 GeV, a nearly-isotropic emission at 10 GeV, both consistent with Fermi-LAT observations, and a near-limb emission at 1 TeV. Our model can also reproduce the flux-drop detected by HAWC ( 1 TeV). Finally, we argue that the spectral dip observed at 40 GeV may result from the flux suppression at low energy due to the cross-field diffusion, which would produce a cutoff. These findings underscore the pivotal role of closed magnetic field structures in shaping the solar disk gamma-ray emission.
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