A Connection of Inelasticity With Multiplicity Distribution at High Energies

Golyak, I.G.

doi:10.1142/s0217732392003839

Cited by 8 publications

(6 citation statements)

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“…It is well established experimentally that at very high energies ( √ s 3 GeV) the incoming particles lose only one-half their energy via pion photoproduction independently of the number of pions produced, i.e., y ∼ 1/2 [267]. This leading particle effect is consistent with (126).…”

Section: Opacity Of the Cmb To Uhecr Protonssupporting

confidence: 58%

Ultra High Energy Cosmic Rays

Zepeda¹,

Lopez²,

Villaseñor³

2003

AIP Conference Proceedings

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In this report we review the important progress made in recent years towards understanding the experimental data on ultra-high-energy (E 10 9 GeV) cosmic rays. We begin with a general survey of the available data, including a description of the energy spectrum, the nuclear composition, and the distribution of arrival directions. At this point we also give a synopsis of experimental techniques. After that, we introduce the fundamentals of cosmic ray acceleration and energy loss during propagation, with a view of discussing the conjectured nearby sources. Next, we survey the state of the art regarding the high-and ultra-high-energy cosmic neutrinos which may be produced in association with the observed cosmic rays. These neutrinos could constitute key messengers identifying currently unknown cosmic accelerators, possibly in the distant universe, because their propagation is not influenced by background photon or magnetic fields. Subsequently, we summarize the phenomenology of cosmic ray air showers. We describe the hadronic interaction models used to extrapolate results from collider data to ultra-high energies and the main electromagnetic processes that govern the longitudinal shower evolution. Armed with these two principal shower ingredients and motivation from the underlying physics, we describe the different methods proposed to distinguish the primary particle species. In the end, we explore how ultra-high-energy cosmic rays can be used as probes of beyond standard model physics models.

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Section: Opacity Of the Cmb To Uhecr Protonssupporting

confidence: 58%

Ultra High Energy Cosmic Rays

Zepeda¹,

Lopez²,

Villaseñor³

2003

AIP Conference Proceedings

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show abstract

“…However, it is well established experimentally [247] that, at very high energies ( √ s > ∼ 3 GeV), the incoming particles lose only one-half their energy via pion photoproduction independently of the number of pions produced. This is the "leading particle effect".…”

Section: A the Gzk Cutoffmentioning

confidence: 99%

Ultrahigh Energy Cosmic Rays: The State of the Art Before the Auger Observatory

Anchordoqui

Paul

Reucroft

et al. 2003

Int. J. Mod. Phys. A

117

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In this review we discuss the important progress made in recent years towards understanding the experimental data on cosmic rays with energies ≳ 1019eV. We begin with a brief survey of the available data, including a description of the energy spectrum, mass composition, and arrival directions. At this point we also give a short overview of experimental techniques. After that, we introduce the fundamentals of acceleration and propagation in order to discuss the conjectured nearby cosmic ray sources. We then turn to theoretical notions of physics beyond the Standard Model where we consider both exotic primaries and exotic physical laws. Particular attention is given to the role that TeV-scale gravity could play in addressing the origin of the highest energy cosmic rays. In the final part of the review we discuss the potential of future cosmic ray experiments for the discovery of tiny black holes that should be produced in the earth's atmosphere if TeV-scale gravity is realized in Nature.

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“…For multi-pion production the case is much more complicated because of the non-trivial final state kinematics. However, it is well established experimentally [109] that, at very high energies ( √ s 3 GeV), the incoming particles lose only one-half their energy via pion photoproduction independently of the number of pions produced, y π ∼ 1/2. This is the "leading particle effect".…”

Section: Opacity Of the Cmb To Uhecr Protonsmentioning

confidence: 99%

Ultrahigh Energy Cosmic Rays: Facts, Myths, and Legends

Anchordoqui¹

2011

Preprint

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This is a written version of a series of lectures aimed at graduate students in astrophysics/particle theory/particle experiment. In the first part, we explain the important progress made in recent years towards understanding the experimental data on cosmic rays with energies 10 8 GeV. We begin with a brief survey of the available data, including a description of the energy spectrum, mass composition, and arrival directions. At this point we also give a short overview of experimental techniques. After that, we introduce the fundamentals of acceleration and propagation in order to discuss the conjectured nearby cosmic ray sources, and emphasize some of the prospects for a new (multi-particle) astronomy. Next, we survey the state of the art regarding the ultrahigh energy cosmic neutrinos which should be produced in association with the observed cosmic rays. In the second part, we summarize the phenomenology of cosmic ray air showers. We explain the hadronic interaction models used to extrapolate results from collider data to ultrahigh energies, and describe the prospects for insights into forward physics at the Large Hadron Collider (LHC). We also explain the main electromagnetic processes that govern the longitudinal shower evolution. Armed with these two principal shower ingredients and motivation from the underlying physics, we describe the different methods proposed to distinguish primary species. In the last part, we outline how ultrahigh energy cosmic ray interactions can be used to probe new physics beyond the electroweak scale. §

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A Connection of Inelasticity With Multiplicity Distribution at High Energies

Abstract: The widely known experimental value of the mean coefficient of the inelasticity <K>~0.5 is calculated by the investigation of a connection of the inelasticity with KNO scaling invariant multiplicity distributions of secondary particles.

Cited by 8 publications

References 0 publications

Ultra High Energy Cosmic Rays

Ultra High Energy Cosmic Rays

Ultrahigh Energy Cosmic Rays: The State of the Art Before the Auger Observatory

Ultrahigh Energy Cosmic Rays: Facts, Myths, and Legends

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