Collective behavior in nuclear interactions and shower development

Canoa, V.; Armesto, N.; Pajares, C.; Vázquez, R. A.

doi:10.1016/j.astropartphys.2005.02.005

Cited by 3 publications

(4 citation statements)

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“…12.40.Nn, 96.40.De, 96.40.Pq Most QCD-inspired models of multiparticle production predict, in hadron-hadron and nucleus-nucleus collisions at high energy, an increase with energy of the inelasticity parameter, [6,7]. These models predict large stopping power and a decrease of the momentum fraction carried by fast particles.…”

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confidence: 99%

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Percolation Effects in Very-High-Energy Cosmic Rays

et al. 2006

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Most QCD models of high energy collisions predict that the inelasticity K is an increasing function of the energy. We argue that, due to percolation of strings, this behaviour will change and, at √ s ≃ 10 4 GeV, the inelasticity will start to decrease with the energy. This has straightforward consequences in high energy cosmic ray physics: 1) the relative depth of the shower maximum X grows faster with energy above the knee; 2) the energy measurements of ground array experiments at GZK energies could be overestimated.PACS numbers: 13.87. 12.40.Nn, 96.40.De, 96.40.Pq Most QCD-inspired models of multiparticle production predict, in hadron-hadron and nucleus-nucleus collisions at high energy, an increase with energy of the inelasticity parameter, [6,7]. These models predict large stopping power and a decrease of the momentum fraction carried by fast particles.Two aspects are essential in the String Percolation Model [8,9] that we use here: 1) At low energy (or density) leading valence strings are produced. As the energy increases, energy is drawn from the valence strings to produce, centrally in rapidity, sea strings. As in all the models mentioned above, the inelasticity increases with the energy. 2) At very high energy, above the percolation threshold, percolation leads to the formation of a large cluster of strings and to the production of faster particles. As a consequence the inelasticity starts to decrease with the energy.While the relatively low energy regime, with K increasing, is similar to the models already mentioned, the higher energy regime, with decreasing K and the regeneration of the fast particles, is new and has some straightforward consequences in cosmic ray physics.In the String Percolation Model [8, 9] for hadronhadron collisions, at low energy, valence strings are formed, forward and backward in the centre-of-mass, along the collision axis, containing most of the collision energy. As the energy increases, additional sea strings, central in rapidity, are created, taking away part of the energy carried the valence strings. In the impact parameter plane all the strings look like disks, and we have to deal with a two dimension percolation problem.The relevant parameter in percolation theory is the transverse density, η [10],where r is the transverse radius of the string, R the effective radius of the interaction area. N s , the average number of strings, depends on the density (centrality) and on the energy. The strings may overlap in the interaction area, forming clusters of N strings. If η ≪ 1, the average number of strings per cluster is < N >≃ 1. If η ≫ 1, < N >≃ N s . If n is the particle density for one string, m T the average transverse mass produced from a single string, and there are N s strings, one expects:with a colour summation reduction factor [11,12],The particle density does not increase as fast as N s (this corresponds to the saturation phenomenon [9]), and < m T > slowly increases with energy and density. These features are seen in data (see, for instance, [13]). Following [...

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“…Recently, several papers appeared studying collective and non-linear QCD effects, based on the Colour Glass Condensate Model [4], Reggeon Calculus [5], and Strong Field string Model [6,7]. These models predict large stopping power and a decrease of the momentum fraction carried by fast particles.…”

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Percolation Effects in Very-High-Energy Cosmic Rays

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“…Classes (1)(2)(3) can be expressed in a simple numbers and their effects to the air shower development were systematically discussed in [3]. On the other hand, the effects of (4) and (5) have not been discussed widely because of its complexity ( [4] for the nuclear effect for example).…”

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Review of Accelerator Experiments Relevant to Air Shower Development

Sako

2018

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

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Hadronic interaction models are extensively tested using the LHC data since its beginning in 2009. The paper reviews the LHC results relevant to air shower modeling. Measurements of forward particle productions are especially focused because they carry a large fraction of collision energy. The paper reviews not only the LHC results, but also covers a fixed-target experiment and a lower energy collider experiment. A future possibility of LHC light-ion collisions is also discussed.

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“…Cosmic ray interactions with the atmosphere consist of collisions between nuclei ranging from protons to iron as the projectiles and nitrogen or oxygen as the targets. Precise measurements of proton-nucleus and nucleus-nucleus collisions are mandatory for the correct interpretation of air showers and the determination of their mass composition [12]. Typical nuclear effects such as nuclear shadowing due to rescattering of secondary particles in nuclear medium cause modification of secondary particle spectra.…”

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Monte Carlo study of a new experiment at RHIC measuring the nuclear effect for cosmic ray observations

Suzuki¹,

Itow

Kasahara³

et al. 2017

J. Inst.

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A: We have studied the potential performance of an experiment designed to measure neutral particles emitted in the forward region (η > 6) of proton-nitrogen (p-N) inelastic collisions at √ s N N = 200 GeV. Such measurements will provide for the first time direct information about interactions between proton cosmic rays and the atmosphere at collider energies and will aid in the understanding of the nuclear effect of light-ions in the forward region which is expected to be dominated by the shadowing effect due to rescattering inside nuclear matter; this in turn will allow for the development of better air shower models. We first studied differences among the nuclear effects produced by the interaction models QGSJET II-03, DPMJET 3.04, and EPOS 1.99. We quantified the nuclear effects by calculationg the ratio of energy spectra of p-N collisions and proton-proton (p-p) collisions, which revealed a difference at the 30% level in the forward pion and neutron spectra. In order to assess the expected performance of an experiment designed to measure this difference, a full Monte Carlo calculation was conducted assuming the use of the Relativistic Heavy Ion Collider forward (RHICf) detector at Brookhaven National Laboratory installed at 1,800 cm from the interaction point. We have comfirmed that the detector would be able to identify and measure photons of energies below 100 GeV with position and energy resolutions better than 0.4 mm and 16%, respectively. One can discriminate the nuclear effect incorporated into various interaction models used in air shower simulations by measuring the photon spectrum in two different pseudorapidity ranges: η > 10.5 and 8.8 < η < 10.2.

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Collective behavior in nuclear interactions and shower development

Cited by 3 publications

References 30 publications

Percolation Effects in Very-High-Energy Cosmic Rays

Percolation Effects in Very-High-Energy Cosmic Rays

Review of Accelerator Experiments Relevant to Air Shower Development

Monte Carlo study of a new experiment at RHIC measuring the nuclear effect for cosmic ray observations

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