Closing the net on transient sources of ultra-high-energy cosmic rays
Fuente:
arXiv
Enregistré dans:
| Auteurs principaux: | , , , , |
|---|---|
| Format: | Preprint |
| Publié: |
2024
|
| Sujets: | |
| Accès en ligne: | |
| Tags: |
Ajouter un tag
Pas de tags, Soyez le premier à ajouter un tag!
|
| _version_ | 1866909228593053696 |
|---|---|
| author | Marafico, Sullivan Biteau, Jonathan Condorelli, Antonio Deligny, Olivier Bregeon, Johan |
| author_facet | Marafico, Sullivan Biteau, Jonathan Condorelli, Antonio Deligny, Olivier Bregeon, Johan |
| contents | Arrival directions of ultra-high-energy cosmic rays (UHECRs) observed above $4\times10^{19}\,$eV provide evidence of localized excesses that are key to identifying their sources. We leverage the 3D matter distribution from optical and infrared surveys as a density model of UHECR sources, which are considered to be transient. Agreement of the sky model with UHECR data imposes constraints on both the emission rate per unit matter and the time spread induced by encountered turbulent magnetic fields. Based on radio measurements of cosmic magnetism, we identify the Local Sheet as the magnetized structure responsible for the kiloyear duration of UHECR bursts for an observer on Earth and find that the turbulence amplitude must be within $0.5-20\,$nG for a coherence length of $10\,$kpc. At the same time, the burst-rate density must be above $50\,$Gpc$^{-3}\,$yr$^{-1}$ for Local-Sheet galaxies to reproduce the UHECR excesses and below $5\,000\,$Gpc$^{-3}\,$yr$^{-1}$ ($30\,000\,$Gpc$^{-3}\,$yr$^{-1}$) for the Milky Way (Local-Group galaxies) not to outshine other galaxies. For the transient emissions of protons and nuclei to match the energy spectra of UHECRs, the kinetic energy of the outflows responsible for UHECR acceleration must be below $4\times10^{54}\,$erg and above $5\times10^{50}\,$erg ($2\times10^{49}\,$erg) if we consider the Milky Way (or not). The only stellar-sized transients that satisfy both Hillas' and our criteria are long gamma-ray bursts. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_17179 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Closing the net on transient sources of ultra-high-energy cosmic rays Marafico, Sullivan Biteau, Jonathan Condorelli, Antonio Deligny, Olivier Bregeon, Johan High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics Arrival directions of ultra-high-energy cosmic rays (UHECRs) observed above $4\times10^{19}\,$eV provide evidence of localized excesses that are key to identifying their sources. We leverage the 3D matter distribution from optical and infrared surveys as a density model of UHECR sources, which are considered to be transient. Agreement of the sky model with UHECR data imposes constraints on both the emission rate per unit matter and the time spread induced by encountered turbulent magnetic fields. Based on radio measurements of cosmic magnetism, we identify the Local Sheet as the magnetized structure responsible for the kiloyear duration of UHECR bursts for an observer on Earth and find that the turbulence amplitude must be within $0.5-20\,$nG for a coherence length of $10\,$kpc. At the same time, the burst-rate density must be above $50\,$Gpc$^{-3}\,$yr$^{-1}$ for Local-Sheet galaxies to reproduce the UHECR excesses and below $5\,000\,$Gpc$^{-3}\,$yr$^{-1}$ ($30\,000\,$Gpc$^{-3}\,$yr$^{-1}$) for the Milky Way (Local-Group galaxies) not to outshine other galaxies. For the transient emissions of protons and nuclei to match the energy spectra of UHECRs, the kinetic energy of the outflows responsible for UHECR acceleration must be below $4\times10^{54}\,$erg and above $5\times10^{50}\,$erg ($2\times10^{49}\,$erg) if we consider the Milky Way (or not). The only stellar-sized transients that satisfy both Hillas' and our criteria are long gamma-ray bursts. |
| title | Closing the net on transient sources of ultra-high-energy cosmic rays |
| topic | High Energy Astrophysical Phenomena Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2405.17179 |