A study of the cores of air showers in the size range 104 to 107 particles

1968 ◽  
Vol 46 (10) ◽  
pp. S30-S32 ◽  
Author(s):  
A. M. Bakich ◽  
D. Melley ◽  
C. B. A. McCusker ◽  
D. Nelson ◽  
L. S. Peak ◽  
...  
Keyword(s):  
Transverse Momentum ◽  
Size Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Air Showers ◽  
Shower Size ◽  
Charge Spectrum ◽  
Very High Energy ◽  
The Mean ◽  
Very High

Results from the Sydney 64-scintillator array are reported. The array now uses logarithmic amplifiers with a range from 1 to 300 000 particles per square meter. This allows us to detect both higher and lower central densities than was previously possible. Further observations and comparison with Monte Carlo calculations confirm the previous result that air showers in the size range 104 to 5 × 105 particles are due to cosmic-ray primaries with much the same charge spectrum as at 1011 eV total energy.Showers of size greater than 106 particles seem mostly to be multicored (in agreement with previous results). The apparent transverse momentum is high and increases with shower size. The quantity rpL/n, which is a measure of the mean transverse momentum in very high energy interactions, is always greater than 1 GeV/c and increases with shower size. The existence and nature of a possible superstrong interaction are briefly discussed.

Lateral distribution and energy spectra of high-energy muons in cosmic-ray air showers

1990 ◽  
Vol 68 (1) ◽  
pp. 41-48 ◽  
Author(s):  
D. K. Basak ◽  
S. K. Sarkar ◽  
N. Mukherjee ◽  
S. Sanyal ◽  
B. Ghosh ◽  
...  
Keyword(s):  
Size Range ◽  
Detection Efficiency ◽  
Cosmic Ray ◽  
High Energy ◽  
Lateral Distribution ◽  
Energy Spectra ◽  
Recent Experimental Data ◽  
Air Showers ◽  
Shower Size ◽  
Primary Composition

The energy spectra and the lateral distribution of muons in cosmic-ray air showers, in the size range 104–106 particles as measured by two magnetic spectrographs each of full detection efficiency for muons in the energy range 2.5–500 GeV, are presented along with the derived muon size vs. shower size results. Comparisons with similar recent experimental data and calculations are given to infer the cosmic-ray primary composition.

scholarly journals Recent Results from the CANGAROO Project

1996 ◽  
Vol 160 ◽  
pp. 363-364
Author(s):  
S.A. Dazeley ◽  
P.G. Edwards ◽  
J.R. Patterson ◽  
G.P. Rowell ◽  
M. Sinnott ◽  
...  
Keyword(s):  
Gamma Rays ◽  
South Australia ◽  
Cosmic Ray ◽  
High Energy ◽  
Relativistic Electrons ◽  
Large Numbers ◽  
Inverse Compton ◽  
Very High Energy ◽  
Large Telescopes ◽  
Very High

TheCollaboration ofAustralia andNippon for aGAmmaRayObservatory in theOutback operates two large telescopes at Woomera (South Australia), which detect the Čerenkov light images produced in the atmosphere by electronpositron cascades initiated by very high energy (~1 TeV or 1012eV) gamma rays. These gamma rays arise from a different mechanism than at EGRET energies: inverse Compton (IC) emission from relativistic electrons.The spoke-like images are recorded by a multi-pixel camera which facilitates the rejection of the large numbers of oblique and ragged cosmic ray images. A field of view ~3.5° is required. The Australian team operates a triple 4 m diameter mirror telescope, BIGRAT, with a 37 photomultiplier tube camera and energy threshold 600 GeV. The Japanese operate a single, highly accurate 3.8 m diameter f/1 telescope and high resolution 256 photomultipler tube camera. In 1998 a new 7 m telescope is planned for Woomera with a design threshold ~;200GeV.

scholarly journals Calculation of the TeV prompt muon component in very high energy cosmic ray showers

1996 ◽  
Vol 4 (4) ◽  
pp. 351-363 ◽  
Author(s):  
G BATTISTONI ◽  
C BLOISE ◽  
C FORTI ◽  
M GRECO ◽  
J RANFT ◽  
...  
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Muon Component ◽  
Very High Energy ◽  
Very High

Search for very high-energy neutrinos by SHALON (Cherenkov radiation of extensive air showers observed at large zenith angles)

2006 ◽  
Vol 151 (1) ◽  
pp. 493-496
Author(s):  
V.G. Sinitsyna ◽  
T.P. Arsov ◽  
S.S. Borisov ◽  
F.I. Musin ◽  
S.I. Nikolsky ◽  
...  
Keyword(s):  
Cherenkov Radiation ◽  
High Energy ◽  
Extensive Air Showers ◽  
Air Showers ◽  
Very High Energy ◽  
High Energy Neutrinos ◽  
Very High

scholarly journals Particle production in very-high-energy cosmic-ray emulsion chamber events: Usual and unusual events

1995 ◽  
Vol 52 (7) ◽  
pp. 3890-3893 ◽  
Author(s):  
C. G. S. Costa ◽  
F. Halzen ◽  
C. Salles
Keyword(s):  
Particle Production ◽  
Cosmic Ray ◽  
High Energy ◽  
Emulsion Chamber ◽  
Very High Energy ◽  
Very High

Two Kinds of Very High Energy Cosmic-Ray Stars

1949 ◽  
Vol 76 (8) ◽  
pp. 1273-1274 ◽  
Author(s):  
L. Leprince-Ringuet ◽  
F. Bousser ◽  
Hoang-Tchang-Fong ◽  
L. Jauneau ◽  
D. Morellet
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Very High Energy ◽  
Very High

The Transition Effect for Large Bursts of Cosmic-Ray Ionization and the Number of Primary Electrons of Very High Energy

1939 ◽  
Vol 56 (7) ◽  
pp. 640-643 ◽  
Author(s):  
C. G. Montgomery ◽  
D. D. Montgomery
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Transition Effect ◽  
Very High Energy ◽  
Primary Electrons ◽  
Very High

scholarly journals Performance optimization of the air shower simulation program for the Cherenkov Telescope Array

2019 ◽  
Vol 214 ◽  
pp. 05041 ◽  
Author(s):  
Luisa Arrabito ◽  
Konrad Bernlöhr ◽  
Johan Bregeon ◽  
Gernot Maier ◽  
Philippe Langlois ◽  
...  
Keyword(s):  
Performance Optimization ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Telescope Array ◽  
Cherenkov Telescope ◽  
Cpu Time ◽  
Very High Energy ◽  
Under Construction ◽  
Very High

The Cherenkov Telescope Array (CTA), currently under construction, is the next-generation instrument in the field of very high energy gamma-ray astronomy. The first data are expected by the end of 2018, while the scientific operations will start in 2022 for a duration of about 30 years. In order to characterize the instrument response to the Cherenkov light emitted when cosmic ray showers develop in the atmosphere, detailed Monte Carlo simulations will be regularly performed in parallel to CTA operation. The estimated CPU time associated to these simulations is very high, of the order of 200 millions HS06 hours per year. Reducing the CPU time devoted to simulations would allow either to reduce infrastructure cost or to better cover the large phase space. In this paper, we focus on the main computing step (70% of the whole CPU time) implemented in the CORSIKA program, and specifically on the mod-ule responsible for the propagation of Cherenkov photons in the atmosphere. We present our preliminary studies about different options of code optimization, with a particular focus on vectorization facilities (SIMD instructions). Our proposals take care, as automatically as possible, of the hardware portability constraints introduced by the grid computing environment that hosts these simulations. Performance evaluation in terms of running-time and accuracy is provided.

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