Comments on "The impact of Solar magnetic field configurations on the production of gamma rays at the Solar disk'' (arXiv:2512.01403)

TL;DR

This comment compares two studies on solar magnetic fields and gamma-ray production, highlighting their agreements, differences, and how they can complement each other to improve understanding of solar high-energy emissions.

Contribution

It clarifies the relationship between a recent Monte Carlo simulation study and a previous work, emphasizing their combined potential for solar gamma-ray research.

Findings

Both studies model hadronic interactions and magnetic effects similarly.

They agree on some predictions for gamma-ray emissions.

Differences in assumptions highlight areas for joint analysis.

Abstract

In this short comment, I discuss the relationship between the results presented in arXiv:2512.01403 and those previously published in Phys.~Rev.~D~101,~083011~(2020). The 2020 study provides a full Monte Carlo simulation of cosmic-ray interactions with the solar atmosphere using the FLUKA code, including realistic solar-atmosphere models, PFSS/Parker/BIFROST magnetic-field configurations, and predictions for gamma rays, electrons, positrons, neutrons, and neutrinos. Given the substantial scientific overlap -- particularly in the modelling of hadronic interactions, magnetic-field effects, cascade development, and comparison with Fermi-LAT observations -- a direct comparison is relevant to assess consistency and complementarity. Here I summarize the main points of agreement, highlight differences in modeling assumptions, and outline how the two approaches can jointly contribute to understanding high-energy emission from the solar disk.