Photonuclear interactions of ultrahigh energy cosmic rays and their astrophysical consequences

Puget, J.‐L.; Stecker, F. W.; Bredekamp, J. H.

doi:10.1086/154321

Cited by 325 publications

(466 citation statements)

References 18 publications

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“…Photo-disintegration of nuclei with large mass number A is dominated by the giant dipole resonance (GDR) with main branches A → (A − 1) + N and A → (A − 2) + 2N where N indicates a proton or neutron [15][16][17]. The GDR peak in the rest frame of the nucleus lies at about 20 MeV for one-nucleon emission, corresponding to E A GDR A × 2 × −1 meV × 10 10 GeV in the cosmic frame with photon energies = meV meV.…”

Section: Propagation Of Cosmic Ray Nucleimentioning

confidence: 99%

“…For simplicity, we follow the work of Puget, Stecker & Bredekamp (PSB) [16] and consider only one stable isotope per mass number A in the decay chain of 56 Fe. At energies below 10 MeV in the rest frame of the nucleus there exist typically a number of discrete excitation levels that can become significant for low mass nuclei.…”

Section: Propagation Of Cosmic Ray Nucleimentioning

confidence: 99%

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Cosmogenic gamma rays and the composition of cosmic rays

Ahlers

Salvadó

2011

Phys. Rev. D

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We discuss the prospects of detecting the sources of ultra-high energy (UHE) cosmic ray (CR) nuclei via their emission of cosmogenic γ-rays in the GeV to TeV energy range. These γ-rays result from electromagnetic cascades initiated by high energy photons, electrons and positrons that are emitted by CRs during their propagation in the cosmic radiation background and are independent of the simultaneous emission of γ-rays in the vicinity of the source. The corresponding production power by UHE CR nuclei (with mass number A and charge Z) is dominated by pion photo-production (∝ A) and Bethe-Heitler pair production (∝ Z 2 ). We show that the cosmogenic γ-ray signal from a single steady UHE CR source is typically more robust with respect to variations of the source composition and injection spectrum than the accompanying signal of cosmogenic neutrinos. We study the diffuse emission from the sum of extragalactic CR sources as well as the point source emission of the closest sources.

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Section: Propagation Of Cosmic Ray Nucleimentioning

confidence: 99%

Section: Propagation Of Cosmic Ray Nucleimentioning

confidence: 99%

Cosmogenic gamma rays and the composition of cosmic rays

Ahlers

Salvadó

2011

Phys. Rev. D

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“…This process was studied in details in [25,26]. Starting from the results presented in those papers, some of us derived the neutron production rate due to the PD of nuclei onto a thermal background of photons at the temperature T [24].…”

Section: Neutrons From Nuclei Photo-disintegrationmentioning

confidence: 99%

TeV neutrinos from supernova remnants embedded in giant molecular clouds

Cavasinni

Grasso

Maccione

2006

Astroparticle Physics

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The recent detection of γ-rays with energy up to 10 TeV from dense regions surrounding some Supernova Remnants (SNR) provides strong, though still not conclusive, evidence that the nucleonic component of galactic Cosmic Rays is accelerated in the supernova outflows. Neutrino telescopes could further support the validity of such scenario by detecting neutrinos coming from the same regions. We re-evaluate the TeV range neutrino-photon flux ratio to be expected from pion decay, finding small differences respect to previous derivations. We apply our results and the recent HESS measurements of the very high energy γ-ray flux from the molecular cloud complex in the Galactic Centre, to estimate the neutrino flux from that region discussing the detectability perspectives for Mediterranean Neutrino Telescopes. We also discuss under which conditions neutron decay may give rise to a significant TeV antineutrino flux from a SNR embedded in Molecular Cloud complexes.

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“…The propagation of UHECR protons 2 is affected almost only by the CMB radiation field and the processes that influence the propagation are: (i) pair production and (ii) photo-pion production [15,16]. On the other hand, the propagation of heavier nuclei is affected also by the EBL and the interaction processes relevant are: (i) pair production and (ii) photo-disintegration [13,14,17,18].…”

Section: Secondary Cosmogenic Neutrinosmentioning

confidence: 99%

Ultra High Energy Cosmic Rays and Neutrinos

Aloisio

2016

Nuclear and Particle Physics Proceedings

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We discuss the production of ultra high energy neutrinos coming from the propagation of ultra high energy cosmic rays and in the framework of top-down models for the production of these extremely energetic particles. We show the importance of the detection of ultra high energy neutrinos that can be a fundamental diagnostic tool to solve the discrepancy in the observed chemical composition of ultra high energy cosmic rays and, at the extreme energies, can unveil new physics in connection with the recent cosmological observations of the possible presence of tensor modes in the fluctuation pattern of the cosmic microwave background.

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Photonuclear interactions of ultrahigh energy cosmic rays and their astrophysical consequences

Cited by 325 publications

References 18 publications

Cosmogenic gamma rays and the composition of cosmic rays

Cosmogenic gamma rays and the composition of cosmic rays

TeV neutrinos from supernova remnants embedded in giant molecular clouds

Ultra High Energy Cosmic Rays and Neutrinos

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