Inelasticity in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>p</mml:mi></mml:math>-nucleus collisions and its application to high energy cosmic-ray cascades

Frichter, George M.; Gaisser, T. K.; Stanev, T.

doi:10.1103/physrevd.56.3135

Cited by 30 publications

(31 citation statements)

References 46 publications

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“…In the 1-100 TeV primary energy range, their predictions for p-air are quite similar, while there are larger differences for the estimates of the rate of diffraction processes and for the inelasticity of proton air interactions [53,54]. This last quantity essentially gives the fraction of energy available for particle production [55][56][57] and is particularly important for the longitudinal development of the shower in the atmosphere. Actually the two models that show the largest differences among them are QGSJET-I and SIBYLL-2.1, while QGSJET-II.03 gives predictions closer to those of SIBYLL-2.1 (see for instance [58]).…”

Section: Analysis Results and Discussionmentioning

confidence: 97%

Proton-air cross section measurement with the ARGO-YBJ cosmic ray experiment

Aielli¹,

Bacci²,

Bartoli³

et al. 2009

Phys. Rev. D

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The proton-air cross section in the energy range 1-100 TeV has been measured by the ARGO-YBJ cosmic ray experiment. The analysis is based on the primary cosmic ray flux attenuation for different atmospheric depths (i.e. zenith angles) and exploits the detector capabilities of selecting the shower development stage by means of hit multiplicity, density and lateral profile measurements at ground. The effects of shower fluctuations, the contribution of heavier primaries and the uncertainties of the hadronic interaction models, have been taken into account. The results have been used to estimate the total protonproton cross section at center-of-mass energies between 70 and 500 GeV, where no accelerator data are currently available.

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Section: Analysis Results and Discussionmentioning

confidence: 97%

Proton-air cross section measurement with the ARGO-YBJ cosmic ray experiment

Aielli¹,

Bacci²,

Bartoli³

et al. 2009

Phys. Rev. D

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“…n) occurs around 40% of the time at accelerator energies (Dao et al 1974;Engler et al 1975;Flauger & Mönning 1976;Blobel et al 1978;Forti et al 1990;Frichter et al 1997) and this fraction is predicted by Gribov-Regge theory and Monte Carlo modeling to be only very weakly energy dependent 9 The IBIS telescope on board INTEGRAL has also recently released a preliminary result for the detection of a GC source in the EGRET energy range ( Di Cocco et al 2004). Werner 1993;Engel 2001;Huang et al 2002;Ostapchenko 2003).…”

Section: Detailed Calculation Of Neutron Flux From P-p Collisionsmentioning

confidence: 99%

“…Hence, we take the leading neutron multiplicity, m n , to be given by a fixed proportion of 0.4 (i.e., 40% of all p-p interactions involve charge exchange, independent of incoming proton energy). Further, the highest energy experimental data available indicate, for p-p interactions, an averaged leading neutron elasticity of hx n i ¼ 0:25 (Frichter et al 1997).…”

Section: Detailed Calculation Of Neutron Flux From P-p Collisionsmentioning

confidence: 99%

The AGASA and SUGAR Anisotropies and TeV Gamma Rays from the Galactic Center: A Possible Signature of Extremely High Energy Neutrons

Crocker

Fatuzzo

Jokipii

et al. 2005

ApJ

112

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Recent analysis of data sets from two extensive air shower cosmic-ray detectors shows tantalizing evidence of an anisotropic overabundance of cosmic rays toward the Galactic center region that ''turns on'' around 1018 eV. We demonstrate that the anisotropy could be due to neutrons created in the Galactic center region through charge exchange in proton-proton collisions, where the incident, high-energy protons obey a $E À2 power law associated with acceleration at a strong shock. We show that the normalization supplied by the gamma-ray signal from EGRET GC source 3EG J1746À2851 (ascribed to p-p-induced neutral pion decay at GeV energies), together with a very reasonable spectral index of 2.2, predicts a neutron flux at $10 18 eV fully consistent with the extremely high energy cosmic-ray data. Likewise, the normalization supplied by the very recent GC data from the HESS air Cerenkov telescope at $TeV energies is almost equally compatible with the $10 18 eV cosmic-ray data. Interestingly, however, the EGRET and HESS data appear to be themselves incompatible. We find a plausible resolution of this discrepancy in an effective two-source model. Finally, we argue that the shock acceleration is probably occurring in the shell of Sagittarius A East, an unusual supernova remnant located very close to the Galactic center. In support of this contention we note that (1) the extended shell of this object could provide both of the sources suggested by the gamma-ray data and (2) the unusually strong magnetic field at this remnant, together with a perpendicular shock geometry, allow for acceleration of protons up to the extreme energies required to explain the cosmic-ray anisotropy. If the connection between the anisotropy and Sagittarius A East could be firmly established, it would be the first direct evidence for a particular Galactic source of cosmic rays up to energies near 10 19 eV.

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“…Their results for a QCD pomeron with an asymptotic intercept ∆ = 0.097 are presented, these cross-sections are slightly larger than those for model 3. Also Frichter et al (1997) extrapolate results from accelerator measurements to high energies. They use relative low inelasticities and in turn obtain cross-sections larger as the previous model.…”

Section: Inelastic Cross-sectionsmentioning

confidence: 99%

On total inelastic cross sections and the average depth of the maximum of extensive air showers

Hoerandel¹

2003

J. Phys. G: Nucl. Part. Phys.

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Abstract. The model dependence of the development of extensive air showers generated by high-energy cosmic-ray particles in the atmosphere is studied. The increase of proton-proton and proton-air inelastic cross-sections and values for the elasticity are varied in the hadronic interaction model QGSJET. Using the CORSIKA simulation program, the impact of these changes is investigated on air shower observables like the average depth of the shower maximum Xmax and the number of muons and electrons at ground level. Calculating the mean logarithmic mass from experimental Xmax values, it is found that a moderate logarithmic increase of the proton-proton inelastic cross-section from σ inel pp = 51 mb at E 0 = 10 6 GeV to σ inel pp = 64 mb at E 0 = 10 8 GeV and an elasticity, additionally increased by 10% to 15%, describes the data best. Using these parameters, the mean logarithmic mass ln A derived from Xmax measurements is compatible with the extrapolations of the results of direct measurements to high energies using the poly-gonato model.

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Inelasticity inp-nucleus collisions and its application to high energy cosmic-ray cascades

Cited by 30 publications

References 46 publications

Proton-air cross section measurement with the ARGO-YBJ cosmic ray experiment

Proton-air cross section measurement with the ARGO-YBJ cosmic ray experiment

The AGASA and SUGAR Anisotropies and TeV Gamma Rays from the Galactic Center: A Possible Signature of Extremely High Energy Neutrons

On total inelastic cross sections and the average depth of the maximum of extensive air showers

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