Total Proton-Proton Cross Section at<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi>s</mml:mi></mml:mrow><mml:mrow><mml:mfrac><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mn>2</mml:mn></mml:mrow></mml:mfrac></mml:mrow></mml:msup></mml:mrow><mml:mo>=</mml:mo><mml:mn>30</mml:mn><mml:mn /></mml:math>TeV

Baltrusaitis, R. M.; Cassiday, G. L.; Elbert, J. W.; Gerhardy, P. R.; Ko, S.; Loh, E. C.; Mizumoto, Y.; Sokolsky, P.; Steck, D.

doi:10.1103/physrevlett.52.1380

Cited by 207 publications

(236 citation statements)

References 8 publications

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“…(Kopeliovich et al 1989), (Engel et al 1998), or (Block et al 2000). For example, using a different value for k in equation (2), total inelastic cross-sections obtained by Baltrusaitis et al (1984) and Honda et al (1993) The subsequent conversion of proton-air to proton-proton cross-sections depends on theoretical uncertainties as well. The details required to apply Glauber theory in this context have been discussed by as well as by Wibig and Sobczyńska (1998).…”

Section: Inelastic Cross-sectionsmentioning

confidence: 99%

“…2) For a fixed primary energy and zenith angle the distribution of the average depth of the shower maximum has an exponential tail with a slope given by the attenuation length Λ, see e.g. (Baltrusaitis et al 1984) or (Gaisser et al 1993).…”

Section: Inelastic Cross-sectionsmentioning

confidence: 99%

“…Particle numbers measured with the EAS-TOP experiment have been used to deduce a value for the inelastic proton-air cross-section at knee energies (Aglietta et al 1997). At the highest energies σ inel p−air has been derived from the shower attenuation length Λ by the Fly's Eye experiment (Baltrusaitis et al 1984) using the exponential tail of X max distributions and by the AGASA experiment (Honda et al 1993) measuring particle numbers at ground level. Dyakonov et al (1990) derived lower limits for cross-sections from investigations of the Yakutsk data, applying two methods, fits to the exponential tail of X max and observing the zenith angle distribution of the shower intensity for fixed energies.…”

Section: Inelastic Cross-sectionsmentioning

confidence: 99%

See 2 more Smart Citations

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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Section: Inelastic Cross-sectionsmentioning

confidence: 99%

Section: Inelastic Cross-sectionsmentioning

confidence: 99%

Section: Inelastic Cross-sectionsmentioning

confidence: 99%

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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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“…14. Inelastic proton-air cross sections as a function of energy, according to experimental data (Mielke et al, 1994;Yodh et al, 1983;Gaisser, et al, 1987;Baltrusaitis et al, 1984;Honda et al, 1993;Aglietta et al, 1997) and according to the models in the CORSIKA and MOCCA Monte Carlo Programs. VENUS (Werner, 1993), HDPM (Capdevielle, 1989) and DPMJET (Ranft, 1995) are the hadronic interaction models at high energies provided in the CORSIKA Monte Carlo Program.…”

Section: Longitudinal Development Of Proton Iron and Gamma-ray Primmentioning

confidence: 99%

Observations and implications of the ultrahigh-energy cosmic rays

2000

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The authors define ''ultrahigh-energy cosmic rays'' (UHECRs) as those cosmic rays with energies above 10 18 eV. It had been anticipated that there would be a cutoff in the energy spectrum of primary cosmic rays around 6ϫ10 19 eV induced by the interaction of the particles with the 2.7-K primordial photons. However, recent experimental data have established that particles exist with energies greatly exceeding this. It follows that the sources of such particles are probably nearby, on a cosmological scale. However, although the trajectories of such energetic particles through the galactic and intergalactic magnetic fields may be nearly rectilinear, no astronomical sources have as yet been identified. This is the enigma of the highest-energy cosmic rays. The paper reviews the history of research in this energy regime and critically assesses the observational results on the energy spectrum, arrival directions, and composition of the primary cosmic rays based on observations made by six experiments. The detection methods currently available are described. Special techniques have been developed as particles of 10 20 eV or higher occur at a rate of only about 1 per km 2 per century. Errors in measurement are given particular attention. The authors also review the theoretical predictions for a number of candidate sources of cosmic rays beyond the predicted cutoff. Finally, the four major projects planned to address the question of the origin of UHECRs are briefly described. CONTENTS

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“…The recent result from LHC is also shown by the star marker [26]. The results by cosmic ray detectors are also included [24,[27][28][29][30]. The solid line is the QCD inspired fit [20], the dashed line is the COMPETE collaboration fit [21] and the dotted line is the L γ fit by Menon and Silva [22] .…”

Section: Proton -Air Total Cross Sectionmentioning

confidence: 99%

\(\langle X_{\text{max}} \rangle \) Uncertainty from Extrapolation of Cosmic Ray Air Shower Parameters

Abbasi

Thomson

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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In this work we investigate the uncertainties in the prediction of the average shower maximum, < X max >, by the currently used high energy cosmic ray shower simulation models. Recent measurements at the LHC have provided constrains on some of the parameters in these models. However, uncertainties in the prediction of < X max > remain due to extrapolation from accelerator data up to center of mass of 250 TeV. The extrapolation in the elasticity, multiplicity, and p-p cross section from the LHC energy range to 3 × 10 19 eV in a cosmic ray's lab frame is investigated in this proceeding. Our calculation of the uncertainty in < X max > is approximately equal to the difference among the modern models being used in the field.

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Total Proton-Proton Cross Section ats12=30TeV

Cited by 207 publications

References 8 publications

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

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

Observations and implications of the ultrahigh-energy cosmic rays

\(\langle X_{\text{max}} \rangle \) Uncertainty from Extrapolation of Cosmic Ray Air Shower Parameters

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