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Escape and propagation of UHECR protons and neutrons from GRBs, and the cosmic ray-neutrino connection
High Energy Astrophysical Phenomena · Submitted 12 Jun 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In addition, the extra direct escape component enhances the high-energy part of the UHECR flux, thus improving the agreement between the predictions and the observed flux.
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The abstract, sentence by sentence
We present a model of ultra-high-energy cosmic ray (UHECR) production in the shock-accelerated fireball of a gamma-ray burst. In addition to the standard UHECR origin from neutron escape and decay into protons, our model considers direct proton emission through leakage from the edges of the accelerated baryon-loaded shells that make up the fireball. Depending on the optical thickness of the shells to photohadronic interactions, the source falls in one of three scenarios: the usual, optically thin source dominated by neutron escape, an optically thick source to neutron escape, or a "direct escape" scenario, where the main contribution to UHECRs comes from the leaked protons. The associated neutrino production will be different for each scenario, and we see that the standard "one neutrino per cosmic ray" assumption is valid only in the optically thin case, while more than one neutrino per cosmic ray is expected in the optically thick scenario. In addition, the extra direct escape component enhances the high-energy part of the UHECR flux, thus improving the agreement between the predictions and the observed flux.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a model of ultra-high-energy cosmic ray (UHECR) production in the shock-accelerated fireball of a gamma-ray burst. | contribution 0.96 | 0.88 | 0.06 | asserted 0.98 |
| s1 | In addition to the standard UHECR origin from neutron escape and decay into protons, our model considers direct proton emission through leakage from the edges of the accelerated baryon-loaded shells that make up the fireball. | contribution 0.89 | 0.74 | 0.08 | asserted 1.00 |
| s2 | Depending on the optical thickness of the shells to photohadronic interactions, the source falls in one of three scenarios: the usual, optically thin source dominated by neutron escape, an optically thick source to neutron escape, or a "direct escape" scenario, where the main contribution to UHECRs comes from the leaked protons. | method 0.52 | 0.42 | 0.17 | asserted 0.79 |
| s3 | The associated neutrino production will be different for each scenario, and we see that the standard "one neutrino per cosmic ray" assumption is valid only in the optically thin case, while more than one neutrino per cosmic ray is expected in the optically thick scenario. | result 0.95 | 0.88 | 0.29 | asserted 0.97 |
| s4 | In addition, the extra direct escape component enhances the high-energy part of the UHECR flux, thus improving the agreement between the predictions and the observed flux. | result 0.71 | 0.83 | 0.22 | asserted 0.95 |
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The paper
Original abstract
We present a model of ultra-high-energy cosmic ray (UHECR) production in the shock-accelerated fireball of a gamma-ray burst. In addition to the standard UHECR origin from neutron escape and decay into protons, our model considers direct proton emission through leakage from the edges of the accelerated baryon-loaded shells that make up the fireball. Depending on the optical thickness of the shells to photohadronic interactions, the source falls in one of three scenarios: the usual, optically thin source dominated by neutron escape, an optically thick source to neutron escape, or a "direct escape" scenario, where the main contribution to UHECRs comes from the leaked protons. The associated neutrino production will be different for each scenario, and we see that the standard "one neutrino per cosmic ray" assumption is valid only in the optically thin case, while more than one neutrino per cosmic ray is expected in the optically thick scenario. In addition, the extra direct escape component enhances the high-energy part of the UHECR flux, thus improving the agreement between the predictions and the observed flux.
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What this paper does with the arXiv papers it cites
What it cites · 6 sentences without a confident label
Uses the method or tool of 5 papers
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The transport of protons from the sources to Earth is performed by numerically solving a kinetic equation for the comoving proton density $Y$ (in units of GeV$^-1$ cm$^-3$) [ref] : [equation] The first term on the rhs takes care of the energy dilution due to the adiabatic cosmological expansion, with $H(z)$ the Hubble parameter.
Neutrino diagnostics of ultra-high energy cosmic ray protons · UHECR observations · 1.00
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The transport of protons from the sources to Earth is performed by numerically solving a kinetic equation for the comoving proton density $Y$ (in units of GeV$^-1$ cm$^-3$) [ref] : [equation] The first term on the rhs takes care of the energy dilution due to the adiabatic cosmological expansion, with $H(z)$ the Hubble parameter.
GZK Neutrinos after the Fermi-LAT Diffuse Photon Flux Measurement · UHECR observations · 1.00
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Particles from within a shell of thickness $λ_mfp^'$ are able to escape without interacting (“mfp” refers to the mean free path of particles), so that the fraction of escaping particles [ref] is $f_esc ≡V_direct^'/ V_iso^'≃λ_mfp^'/ Δr^'$.
UHECR escape mechanisms for protons and neutrons from GRBs, and the cosmic ray-neutrino connection · Optically thin and thick sources, and direct proton escape · 0.84
Uses data or values from 3 papers
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We have assumed that identical bursts (in the comoving source frame) are distributed in redshift following the GRB rate from Refs. [ref] .
On the normalisation of the cosmic star formation history · UHECR observations · 0.99
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We have assumed that identical bursts (in the comoving source frame) are distributed in redshift following the GRB rate from Refs. [ref] .
The Star Formation Rate in the Reionization Era as Indicated by Gamma-ray Bursts · UHECR observations · 0.99
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Putting all of this together, the injection spectrum $Q^'$ of neutrinos and neutrons can be computed, and the corresponding fluence per shell (in units of GeV$^-1$ cm$^-2$) is obtained as [equation] Flavour mixing is implemented for neutrinos, assuming a normal mass hierarchy and the best-fit values of the mixing parameters from Ref. [ref] .
Global analysis of neutrino masses, mixings and phases: entering the era of leptonic CP violation searches · The GRB fireball model · 0.96
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