Solar disk gamma-rays emission via synthetic magnetic field from photosphere to low corona
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| Format: | Preprint |
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2025
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| _version_ | 1866918099805011968 |
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| author | Puzzoni, Eleonora Fraschetti, Federico Kóta, József Giacalone, Joe |
| author_facet | Puzzoni, Eleonora Fraschetti, Federico Kóta, József Giacalone, Joe |
| contents | Gamma-ray emission in the GeV-TeV range from the solar disk is likely to arise from collisions of galactic cosmic rays (GCRs) with solar atmospheric plasma. In a previous study, we demonstrated that closed turbulent magnetic arcades trap efficiently GCRs leading to a gamma-ray flux consistent with the Fermi-HAWC observations (from $\sim 0.1$ GeV to $\sim 1$ TeV). Here, we model a synthetic magnetic field with a static, laminar structure of open field lines in the chromosphere increasingly braiding near the solar surface, with a scale height of $\sim 10^{-2} R_\odot$. The height-dependent increase in magnetic field line braiding is modulated by an exponential scalar function, mimicking the bending of the photo- and chromo-spheric magnetic field revealed by polarimetric observations and reproduced by MHD simulations. Employing 3D test-particle numerical simulations, we investigate how distorted magnetic field lines affect the gamma-rays production by injecting GeV-TeV protons into both magnetically laminar and braided regions. We find that with the chosen spatial resolution this synthetic magnetic field can account for the $> 10$ GeV gamma-ray spectrum observed by Fermi-LAT/HAWC. A rebrightening between approximately $30$ and $100$ GeV (following a $\sim 30$ GeV spectral dip), suggests an enhanced confinement within the photo-/chromospheric layer by a stronger braiding. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2507_15468 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Solar disk gamma-rays emission via synthetic magnetic field from photosphere to low corona Puzzoni, Eleonora Fraschetti, Federico Kóta, József Giacalone, Joe High Energy Astrophysical Phenomena Solar and Stellar Astrophysics Gamma-ray emission in the GeV-TeV range from the solar disk is likely to arise from collisions of galactic cosmic rays (GCRs) with solar atmospheric plasma. In a previous study, we demonstrated that closed turbulent magnetic arcades trap efficiently GCRs leading to a gamma-ray flux consistent with the Fermi-HAWC observations (from $\sim 0.1$ GeV to $\sim 1$ TeV). Here, we model a synthetic magnetic field with a static, laminar structure of open field lines in the chromosphere increasingly braiding near the solar surface, with a scale height of $\sim 10^{-2} R_\odot$. The height-dependent increase in magnetic field line braiding is modulated by an exponential scalar function, mimicking the bending of the photo- and chromo-spheric magnetic field revealed by polarimetric observations and reproduced by MHD simulations. Employing 3D test-particle numerical simulations, we investigate how distorted magnetic field lines affect the gamma-rays production by injecting GeV-TeV protons into both magnetically laminar and braided regions. We find that with the chosen spatial resolution this synthetic magnetic field can account for the $> 10$ GeV gamma-ray spectrum observed by Fermi-LAT/HAWC. A rebrightening between approximately $30$ and $100$ GeV (following a $\sim 30$ GeV spectral dip), suggests an enhanced confinement within the photo-/chromospheric layer by a stronger braiding. |
| title | Solar disk gamma-rays emission via synthetic magnetic field from photosphere to low corona |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.15468 |