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| 001 | 459509 | ||
| 005 | 20250715175711.0 | ||
| 024 | 7 | _ | |a 10.1093/mnras/stac433 |2 doi |
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| 024 | 7 | _ | |a arXiv:2107.04612 |2 arXiv |
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| 082 | _ | _ | |a 520 |
| 088 | _ | _ | |a arXiv:2107.04612 |2 arXiv |
| 088 | _ | _ | |a DESY-21-103 |2 DESY |
| 100 | 1 | _ | |a Rudolph, Annika |0 P:(DE-H253)PIP1032309 |b 0 |e Corresponding author |
| 245 | _ | _ | |a Multi-wavelength radiation models for low-luminosity GRBs, and the implications for UHECRs |
| 260 | _ | _ | |a Oxford |c 2022 |b Oxford Univ. Press |
| 336 | 7 | _ | |a article |2 DRIVER |
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| 336 | 7 | _ | |a Journal Article |b journal |m journal |0 PUB:(DE-HGF)16 |s 1647438728_28787 |2 PUB:(DE-HGF) |
| 336 | 7 | _ | |a ARTICLE |2 BibTeX |
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| 336 | 7 | _ | |a Journal Article |0 0 |2 EndNote |
| 520 | _ | _ | |a We study the prompt phase of low-luminosity Gamma-Ray Bursts (LL-GRBs) as potential source of very-high-energy (VHE) gamma rays and ultra-high-energy cosmic rays (UHECRs).We model the spectral energy distribution of three representative examples (with observed properties similar to GRBs 980425, 100316D and 120714B) self-consistently in a leptonic synchrotron self-Compton (SSC) scenario using the internal shock model for the relativistic outflow. To investigate the conditions under which inverse Compton radiation may lead to a peak in the GeV-TeV range potentially observable in Imaging Atmospheric Cherenkov Telescopes (IACTs), we vary the fraction of the energy budget supplying the magnetic field. As a second step, we determine the maximal energies achievable for UHECR nuclei. Assuming LL-GRBs to power the observed UHECR flux, we derive constraints on the baryonic loading and typical GRB duration by explicitly calculating the contribution of LL-GRBs to the diffuse extragalactic gamma-ray background. We find that LL-GRBs are potential targets for multi-mavelength studies and may be in reach of current/ future IACTs and optical/ UV instruments.For comparable sub-MeV emission and similar jet properties, the multi-wavelength predictions show a strong dependence on the magnetic field: weak (strong) magnetic fields induce high (low) fluxes in the VHE regime and low (high) fluxes in the optical. However, VHE emission might be suppressed by $\gamma \gamma $-absorption close to the source (especially for high magnetic fields) or interactions with the extragalactic background light for redshifts $z > 0.1$.For UHECRs, we find that the maximal energies of iron nuclei (protons) can be as high as $\simeq 10^{11}$~GeV ($10^{10}$~GeV) if the magnetic energy density is large (where we predict a weak VHE component). These high energies are possible by decoupling the production regions of UHECR and gamma-rays in our multi-zone model. Finally, we find basic consistency with the energy budget needed to accommodate the UHECR origin from LL-GRBs. |
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| 650 | _ | 7 | |a cosmic radiation: UHE |2 INSPIRE |
| 650 | _ | 7 | |a cosmic radiation: spectrum |2 INSPIRE |
| 650 | _ | 7 | |a gamma ray: burst |2 INSPIRE |
| 650 | _ | 7 | |a energy: internal |2 INSPIRE |
| 650 | _ | 7 | |a iron: nucleus |2 INSPIRE |
| 650 | _ | 7 | |a gamma ray: background |2 INSPIRE |
| 650 | _ | 7 | |a energy: high |2 INSPIRE |
| 650 | _ | 7 | |a magnetic field: high |2 INSPIRE |
| 650 | _ | 7 | |a energy: density |2 INSPIRE |
| 650 | _ | 7 | |a energy: magnetic |2 INSPIRE |
| 650 | _ | 7 | |a VHE |2 INSPIRE |
| 650 | _ | 7 | |a acceleration |2 INSPIRE |
| 650 | _ | 7 | |a optical |2 INSPIRE |
| 650 | _ | 7 | |a shock waves |2 INSPIRE |
| 650 | _ | 7 | |a messenger |2 INSPIRE |
| 650 | _ | 7 | |a spectral |2 INSPIRE |
| 650 | _ | 7 | |a energy spectrum |2 INSPIRE |
| 650 | _ | 7 | |a synchrotron |2 INSPIRE |
| 650 | _ | 7 | |a decoupling |2 INSPIRE |
| 650 | _ | 7 | |a redshift |2 INSPIRE |
| 650 | _ | 7 | |a Cherenkov counter: atmosphere |2 INSPIRE |
| 650 | _ | 7 | |a imaging |2 INSPIRE |
| 650 | _ | 7 | |a suppression |2 INSPIRE |
| 693 | _ | _ | |0 EXP:(DE-H253)ULTRASAT-20211201 |5 EXP:(DE-H253)ULTRASAT-20211201 |e Ultraviolet Transient Astronomy Satellite |x 0 |
| 693 | _ | _ | |0 EXP:(DE-H253)CTA-20150101 |5 EXP:(DE-H253)CTA-20150101 |e Cherenkov Telescope Array |x 1 |
| 700 | 1 | _ | |a Bosnjak, Zeljka |0 P:(DE-HGF)0 |b 1 |
| 700 | 1 | _ | |a Palladino, Andrea |0 P:(DE-H253)PIP1082506 |b 2 |
| 700 | 1 | _ | |a Sadeh, Iftach |0 P:(DE-H253)PIP1006066 |b 3 |
| 700 | 1 | _ | |a Winter, Walter |0 P:(DE-H253)PIP1021242 |b 4 |
| 773 | _ | _ | |a 10.1093/mnras/stac433 |g Vol. 511, no. 4, p. 5823 - 5842 |0 PERI:(DE-600)2016084-7 |n 4 |p 5823 – 5842 |t Monthly notices of the Royal Astronomical Society |v 511 |y 2022 |x 0035-8711 |
| 856 | 4 | _ | |u https://doi.org/10.1093/mnras/stac433 |
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