Cosmic Clues from Amaterasu: Blazar-Driven Ultrahigh-Energy Cosmic Rays?
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arXiv
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866916845874839552 |
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| author | Das, Saikat Hazra, Srijita Gupta, Nayantara |
| author_facet | Das, Saikat Hazra, Srijita Gupta, Nayantara |
| contents | The detection of the Amaterasu event of energy 244 EeV by the Telescope Array, one of the most energetic ultrahigh-energy cosmic rays (UHECRs; $E\gtrsim0.1$ EeV) observed to date, invites scrutiny of its potential source. We investigate whether the nearby blazar PKS~1717+177 at redshift $z=0.137$, located within $2.5^\circ$ of the reconstructed arrival direction, could explain the event under a proton-primary hypothesis. Using a one-zone jet model, we fit the multiwavelength spectral energy distribution of the source, incorporating both leptonic and hadronic cascade emissions from photohadronic interactions inside the jet. Our model supports a cosmic-ray origin of the very-high-energy ($\varepsilon_γ\gtrsim 100$ GeV) $γ$-ray flux and predicts a subdominant neutrino flux, one order of magnitude lower than from TXS~0506+056. Under Lorentz invariance violation, UHECRs escaping the blazar jet above a specific energy can propagate unattenuated over hundreds of Mpc due to an increase in energy loss length for certain parameter choices. In such a scenario, the Amaterasu event can have a plausible origin from this blazar. Our analysis indicates negligible deflection in the Galactic magnetic field, implying a strong extragalactic magnetic field is required. Our findings provide a compelling multimessenger framework linking UHECRs, $γ$-rays, and neutrinos and motivate targeted searches by current and future high-energy neutrino telescopes during increased $γ$-ray or X-ray activity of this blazar. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_16019 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Cosmic Clues from Amaterasu: Blazar-Driven Ultrahigh-Energy Cosmic Rays? Das, Saikat Hazra, Srijita Gupta, Nayantara High Energy Astrophysical Phenomena The detection of the Amaterasu event of energy 244 EeV by the Telescope Array, one of the most energetic ultrahigh-energy cosmic rays (UHECRs; $E\gtrsim0.1$ EeV) observed to date, invites scrutiny of its potential source. We investigate whether the nearby blazar PKS~1717+177 at redshift $z=0.137$, located within $2.5^\circ$ of the reconstructed arrival direction, could explain the event under a proton-primary hypothesis. Using a one-zone jet model, we fit the multiwavelength spectral energy distribution of the source, incorporating both leptonic and hadronic cascade emissions from photohadronic interactions inside the jet. Our model supports a cosmic-ray origin of the very-high-energy ($\varepsilon_γ\gtrsim 100$ GeV) $γ$-ray flux and predicts a subdominant neutrino flux, one order of magnitude lower than from TXS~0506+056. Under Lorentz invariance violation, UHECRs escaping the blazar jet above a specific energy can propagate unattenuated over hundreds of Mpc due to an increase in energy loss length for certain parameter choices. In such a scenario, the Amaterasu event can have a plausible origin from this blazar. Our analysis indicates negligible deflection in the Galactic magnetic field, implying a strong extragalactic magnetic field is required. Our findings provide a compelling multimessenger framework linking UHECRs, $γ$-rays, and neutrinos and motivate targeted searches by current and future high-energy neutrino telescopes during increased $γ$-ray or X-ray activity of this blazar. |
| title | Cosmic Clues from Amaterasu: Blazar-Driven Ultrahigh-Energy Cosmic Rays? |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.16019 |