The nature of the asymmetrical showers at an energy of 200 GeV and the features of the pion interaction

1968 ◽  
Vol 46 (10) ◽  
pp. S681-S683 ◽  
Author(s):  
I. N. Erofeeva ◽  
L. G. Mishchenko ◽  
V. S. Murzin ◽  
L. I. Sarycheva
Keyword(s):  
Pion Mass ◽  
Center Of Mass ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Mass System ◽  
Target Mass ◽  
Considerable Portion ◽  
Pion Interaction ◽  
200 Gev ◽  
Ionization Calorimeter

The nuclear interactions of nucleons and pions at an energy of 200 GeV have been studied using an ionization calorimeter, cloud chamber, and hodoscope units. It has been found that the showers which are asymmetrical backward have the two-peak angular distribution (on a log tan θ plot) and, in the center-of-mass system, the charged particles and neutrals appear in the remote and front hemispheres respectively. The showers which are asymmetrical forward are produced mainly by primary pions and are symmetrical in the system where the target mass is close to the pion mass. It is suggested that in the cosmic-ray energy range (e.g. at energies ~10 GeV), after interaction, a pion retains a considerable part of the primary energy, but may change its charge and be transmuted into a π0 meson. Such an assumption makes it possible to explain the considerable portion of the energy transferred to a photon in the pion interactions.

scholarly journals Very high energy cosmic gamma rays

1965 ◽  
Vol 23 ◽  
pp. 253-258
Author(s):  
M. Libber ◽  
S. N. Milford ◽  
M. S. Spergel
Keyword(s):  
Pion Production ◽  
Center Of Mass ◽  
Cosmic Ray ◽  
High Energy ◽  
Mass System ◽  
Proton Proton ◽  
Production Spectrum ◽  
Very High Energy ◽  
Γ Rays ◽  
Γ Ray

Collisions of high energy cosmic rays with intergalactic gas produce various secondaries, including neutral pions that decay into high energy γ rays. The Landau-Milekhin hydrodynamical model for proton-proton collisions is used to calculate the pion production spectrum corresponding to cosmic γ rays of energy above 10 Gev. A source function for these high energy γ rays in space is found by combining the pion production and decay spectra with the primary cosmic ray proton flux. The resulting γ ray spectrum follows a different power law than spectra based upon the usual assumption of a line spectrum for the pions in the center of mass system of the colliding protons. The high energy γ ray intensity in space is calculated for a simple model universe. By comparison with previous estimates for the proton photoproduction process, it is found that proton-proton and proton-photon collisions appear to contribute about the same order of magnitude to the intergalactic γ ray intensity above ∼1016 eV.

scholarly journals INFLUENCE OF THE RESULTS OF UHECR DETECTION ON THE LHC EXPERIMENTS

2013 ◽  
Vol 53 (A) ◽  
pp. 707-711 ◽  
Author(s):  
Anatoly A. Petrukhin
Keyword(s):  
Experimental Data ◽  
Cosmic Rays ◽  
Energy Region ◽  
Center Of Mass ◽  
Cosmic Ray ◽  
Theoretical Models ◽  
Energy Interval ◽  
Mass System ◽  
New Approaches ◽  
Region 10

The cosmic ray energy region 10<sup>15</sup> ÷ 10<sup>17</sup>TeV corresponds to LHC energies 1 ÷ 14TeV in the center-of-mass system. The results obtained in cosmic rays (CR) in this energy interval can therefore be used for developing new approaches to the analysis of experimental data, for interpreting the results, and for planning new experiments. The main problem in cosmic ray investigations is the remarkable excess of muons, which increases with energy and cannot be explained by means of contemporary theoretical models. Some possible new explanations of this effect and other unusual phenomena observed in CR, and ways of searching for them in the LHC experiments are discussed.

Characteristics of clusters produced in nucleon–nucleus interactions at ultrahigh energies

1989 ◽  
Vol 67 (2-3) ◽  
pp. 119-127 ◽  
Author(s):  
D. P. Goyal ◽  
Animesh Kumar ◽  
K. Yugindro Singh ◽  
S. Singh
Keyword(s):  
Cross Section ◽  
Cluster Size ◽  
Channel Model ◽  
Charged Particles ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Target Mass ◽  
Rapidity Gap ◽  
Cluster Density ◽  
The Cross

The phenomenon of cluster production in nucleon–nucleus interactions at ultrahigh energies [Formula: see text] has been investigated using the available cosmic-ray data. The rapidity gap distributions of charged particles in a nondiffractive region of the cross section are found to support the Snider two-channel model as opposed to the model of Quigg, Pirilla, and Thomas. The variation of cluster density and cluster size with the primary energy, multiplicity of shower particles, and nature of the target mass has also been studied.

HELICITY AMPLITUDES FOR COLLIDING BEAM SCATTERING OF TWO SPIN 1/2 PARTICLES

1993 ◽  
Vol 08 (30) ◽  
pp. 5383-5407
Author(s):  
T.B. ANDERS ◽  
A.O. BARUT ◽  
W. JACHMANN
Keyword(s):  
Center Of Mass ◽  
Mass System ◽  
Intermediate Transformation ◽  
Beam System ◽  
Pair Annihilation ◽  
Helicity Amplitudes ◽  
Reaction Channels ◽  
Invariant Coupling ◽  
Exchange Scattering ◽  
The One

As a generalization and extension of the extensive tables of polarization asymmetries given in a previous work,1 we present here tables of helicity amplitudes for the scattering of two spin 1/2 particles in the colliding beam system (i.e. two incoming particles with opposite directions but not necessarily of equal momenta). The particles belonging to the same current may have different masses in order to describe particle excitations. The amplitudes are given for six different basic couplings connecting two vector vertices, a vector vertex at the one current and a derivative vector vertex at the other current, two derivative vector vertices, two tensor vertices, and two scalar vertices. The vertices include axial couplings by factors of type 1+cγ5. The amplitudes are written as expressions with 16 components in the six different reaction channels, namely the scattering of two fermions, of two antifermions, and of a fermion and an antifermion, the pair creation by pair annihilation, as well as the exchange scattering for two identical fermions or antifermions. The formulas may be used for an analysis which extracts the invariant coupling functions from the experimental data obtained in the colliding beam system directly without an intermediate transformation to the center of mass system.

Inclusive Single-Particle Production at 90° in the Center-of-Mass System for Nuclear Targets and 28.5-GeV/cIncident Protons

1976 ◽  
Vol 37 (26) ◽  
pp. 1731-1734 ◽  
Author(s):  
U. Becker ◽  
J. Burger ◽  
M. Chen ◽  
G. Everhart ◽  
F. H. Heimlich ◽  
...  
Keyword(s):  
Single Particle ◽  
Particle Production ◽  
Center Of Mass ◽  
Mass System ◽  
Nuclear Targets

scholarly journals Longitudinal profiles of Extensive Air Showers with inclusion of charm and bottom particles

2019 ◽  
Vol 34 (12) ◽  
pp. 1950069
Author(s):  
M. A. Müller ◽  
V. P. Gonçalves
Keyword(s):  
Large Fraction ◽  
Cosmic Ray ◽  
Primary Energy ◽  
Considerable Change ◽  
Extensive Air Showers ◽  
Longitudinal Profile ◽  
Air Showers ◽  
Energy Deposit ◽  
Production Models ◽  
Longitudinal Profiles

Charm and bottom particles are rare in Extensive Air Showers, but their effects can be radical on the EASs development. If such particles show up with a large fraction of primary energy, they can reach large atmospheric depths, depositing energy in deeper layers of the atmosphere. That will cause changes at the EAS observables ([Formula: see text], RMS and [Formula: see text]), besides a considerable change in the shape of longitudinal profile energy deposit in the atmosphere. We are using for this work a modified code of an EAS simulator, CORSIKA, with production of charm and bottom particles at the first interaction of the primary cosmic ray. We will show in this paper some results to different [Formula: see text] values and different production models.

scholarly journals Testing Compound Nucleus Hypothesis Across the 17O Nucleus Excitation

2019 ◽  
Vol 211 ◽  
pp. 02001 ◽  
Author(s):  
Aloys Nizigama ◽  
Pierre Tamagno ◽  
Olivier Bouland
Keyword(s):  
Cross Section ◽  
Compound Nucleus ◽  
Cross Sections ◽  
Center Of Mass ◽  
Ground States ◽  
Mass System ◽  
Resonance Parameters ◽  
Second Stage ◽  
Reference Framework ◽  
Kinetic Transformation

The excited compound nucleus 17O* has been studied over (n,α) and (α,n) cross sections modelling, respectively for 16O and 13C targets in their ground states. The modelling is fulfilled within the Reich-Moore formalism. We were able to calculate the (α,n) cross section by two separate ways: the direct kinematic standard route and by inversion of the (n,α) cross section using the compound nucleus hypothesis. Resonance parameters of the resolved resonance range (0 to 6 MeV) were borrowed from the CIELO project. In a first stage, the modelling is carried out in the referential of the incident particle (either way neutron or α) requesting conversion of the CIELO neutron-type resonance parameters to the α-type. In a second stage, the implementation is uniquely designed in the center of mass system of the excited compound nucleus. The resonance parameters are thus converted in that unique reference framework. The present investigation shows the consistency of the kinetic transformation that relies on the compound nucleus hypothesis.

Measurement of the cosmic-ray iron spectrum between 60 and 200 GeV per nucleon

1990 ◽  
Vol 351 ◽  
pp. 459 ◽  
Author(s):  
Joseph A. Esposito ◽  
Robert E. Streitmatter ◽  
V. K. Balasubrahmanyan ◽  
Jonathan F. Ormes
Keyword(s):  
Cosmic Ray ◽  
200 Gev
Sign in / Sign up

Export Citation Format

Share Document