The Barometric Effect for Large Cosmic-Ray Bursts under Thick Absorbers at 11,500 Feet Elevation and the Absorption Mean Free Path for Very High Energy Nuclear Collisions

1950 ◽  
Vol 80 (3) ◽  
pp. 479-480 ◽  
Author(s):  
Thomas G. Stinchcomb
Keyword(s):  
Free Path ◽  
Cosmic Ray ◽  
Mean Free Path ◽  
High Energy ◽  
Nuclear Collisions ◽  
Very High Energy ◽  
Barometric Effect ◽  
Very High

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

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

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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