Particle Collisions Above 10 TeV as Seen by Cosmic Rays

Gaisser, T. K.; Yodh, G.

doi:10.1146/annurev.ns.30.120180.002355

Cited by 65 publications

(9 citation statements)

References 56 publications

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“…This observation reveals the fact that the accelerator data on Feynman x F distributions in the fragmentation region are relevant for the analysis of secondary cosmic rays on Earth's atmosphere. A recent study supports the earlier observation of Gaisser and Yodh [31], who have shown that the superposition model is approximately applicable to the investigation of A-A collisions in high-energy cosmic-ray propagation. It may be pointed out that the muon fluxes decrease by 20% when corrected for pp collisions due to A-A collisions.…”

Section: Estimated Muon Flux Is Mainly Dependent On Z Asupporting

confidence: 86%

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Muon Fluxes Derived From the Directly Measured Primary Cosmic Ray Elemental Spectra

1996

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The muon energy spectra at 0° and 89° have been estimated from the decay of nonprompt and prompt mesons created by the individual elemental primary cosmic ray groups during nucleus-air collisions in the upper atmosphere and the results are found to be fairly comparable with the measured muon fluxes obtained from the direct magnetic spectrograph results in Refs. 2–4, and also from the underground indirect measurements in Refs. 5–10. The muon spectrum derived from the single slope primary nucleon spectrum with a constant spectral index of value −2.73 is only slightly different from the present result for energies below 20 TeV. The present muon spectra at large zenith angle exhibit steeper spectral indices when compared to the expected results obtained from primary elemental groups by Parente et al.

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Section: Estimated Muon Flux Is Mainly Dependent On Z Asupporting

confidence: 86%

“…-The branching ratios, mass, lifetime of the charmed particles h and the critical energies of the charmed particle decay for pp K h 6 X inclusive reactions producing h charmed mesons through the decay D K K 1 m 1 n and L c K L 1 m 1 n[31].…”

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confidence: 99%

Muon Fluxes Derived From the Directly Measured Primary Cosmic Ray Elemental Spectra

1996

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“…Even though neutrons which are produced in the cascade are not confined by the magnetic field, the amount of gas present is sufficient to prevent them from escaping. The hadronic cascade in the disk is much simpler than cascades in the earth's atmosphere [22,23,24], since the density of the accretion disk is so low that all unstable particles decay rather than interact. Therefore the cascade consists of a nucleonic part which feeds into the mesonic and electromagnetic channels; no pion-nucleon reactions occur.…”

Section: Hadronic Cascadesmentioning

confidence: 99%

Neutrino production through hadronic cascades in AGN accretion disks

Nellen¹,

Mannheim

Biermann

1993

Phys. Rev. D

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We consider the production of neutrinos in active galactic nuclei (AGN) through hadronic cascades. The initial, high energy nucleons are accelerated in a source above the accretion disk around the central black hole. From the source, the particles diffuse back to the disk and initiate hadronic cascades. The observable output from the cascade are electromagnetic radiation and neutrinos. We use the observed diffuse background X-ray luminosity, which presumably results from this process, to predict the diffuse neutrino flux close to existing limits from the Frejus experiment. The resulting neutrino spectrum is E −2 down to the GeV region. We discuss modifications of this scenario which reduce the predicted neutrino flux.

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“…The hadronic cascade in the disk is much simpler than cascades in the earth's atmosphere (Gaisser 1990, Gaisser & Yodh 1980, Gaisser et al 1978, since the density of the accretion disk is so low that all unstable particles decay rather than interact. Therefore the cascade consists of a nucleonic part which feeds into the mesonic and electro-magnetic channels; no pion-nucleon reactions occur.…”

Section: The Hadronic Cascade In the Accretion Diskmentioning

confidence: 99%

Agn and Galactic Sites of Cosmic Ray Origin

Biermann

1994

High Energy Astrophysics

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In the following we review recent progress in our understanding of the physics of energetic particles in our Galaxy, in active galaxies such as starburst galaxies, in active galactic nuclei and in the jets and radio hot spots of powerful radio galaxies and radioloud quasars. We propose that cosmic rays originate mainly in three sites, a) normal supernova explosions into the approximately homogeneous interstellar medium, b) supernova explosions into stellar winds, and c) hot spots of powerful radio galaxies. The predictions based on this proposition have been tested successfully against airshower data over the particle energy range from 10 TeV to 100 EeV. The energy input from supernova explosions in starburst galaxies is so large, as to produce breakouts from the galactic disks, observable most prominently in X-ray and nonthermal radio emission. Normal galaxies are also likely to have winds. The low energy cosmic ray particles carried out by such galactic winds to the intergalactic medium may ionize and heat this medium consistent with all known constraints. Furthermore we propose that radioloud quasars accelerate nuclei to high energies in shocks in the inner sections of their jets, and thus initiate hadronic cascades which produce the γ-ray emission observed with GRO. Radio observations of the Galactic center compact source suggest that there is a jet similar to that in quasars, but very much weaker in its emission; simple modelling suggests that the power carried by this jet is of order similar to the accretion disk luminosity. By analogy we speculate that also radioweak quasars have jets which carry a large proportion of the accretion power, and which accelerate particles to high energy. These energetic particles might serve to heat the inner regions of the host galaxies to produce the strong farinfrared dust emission, and could also initiate hadronic and electromagnetic cascades in the inner accretion disk close to the presumed black hole in the center, to produce a large part of the X-ray emission observed from radioweak AGN.

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Particle Collisions Above 10 TeV as Seen by Cosmic Rays

Cited by 65 publications

References 56 publications

Muon Fluxes Derived From the Directly Measured Primary Cosmic Ray Elemental Spectra

Muon Fluxes Derived From the Directly Measured Primary Cosmic Ray Elemental Spectra

Neutrino production through hadronic cascades in AGN accretion disks

Agn and Galactic Sites of Cosmic Ray Origin

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