Analysis of the hadronic energy spectrum in high-energy cosmic-ray families detected by emulsion chambers

1993 ◽  
Author(s):  
J. Bellandi ◽  
C. G. S. Costa ◽  
R. J. M. Covolan ◽  
C. Dobrigkeit ◽  
M. M. Guzzo ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
High Energy ◽  
Hadronic Energy

scholarly journals The Pierre Auger Observatory: Review of Latest Results and Perspectives

Universe ◽  
2018 ◽  
Vol 4 (11) ◽  
pp. 128 ◽  
Author(s):  
Dariusz Góra ◽  
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
Detection System ◽  
Cosmic Ray ◽  
High Energy ◽  
Pierre Auger Observatory ◽  
Mass Composition ◽  
Ultra High Energy ◽  
Energy Limitation ◽  
Arrival Directions

The Pierre Auger Observatory is the world’s largest operating detection system for the observation of ultra high energy cosmic rays (UHECRs), with energies above 10 17 eV. The detector allows detailed measurements of the energy spectrum, mass composition and arrival directions of primary cosmic rays in the energy range above 10 17 eV. The data collected at the Auger Observatory over the last decade show the suppression of the cosmic ray flux at energies above 4 × 10 19 eV. However, it is still unclear if this suppression is caused by the energy limitation of their sources or by the Greisen–Zatsepin–Kuzmin (GZK) cut-off. In such a case, UHECRs would interact with the microwave background (CMB), so that particles traveling long intergalactic distances could not have energies greater than 5 × 10 19 eV. The other puzzle is the origin of UHECRs. Some clues can be drawn from studying the distribution of their arrival directions. The recently observed dipole anisotropy has an orientation that indicates an extragalactic origin of UHECRs. The Auger surface detector array is also sensitive to showers due to ultra high energy neutrinos of all flavors and photons, and recent neutrino and photon limits provided by the Auger Observatory can constrain models of the cosmogenic neutrino production and exotic scenarios of the UHECRs origin, such as the decays of super heavy, non-standard-model particles. In this paper, the recent results on measurements of the energy spectrum, mass composition and arrival directions of cosmic rays, as well as future prospects are presented.

A Deduction of the High Energy Spectrum of Cosmic-Ray Primary Nucleons from the Observed Muon Spectrum

1951 ◽  
Vol 84 (6) ◽  
pp. 1199-1203 ◽  
Author(s):  
Uri Haber-Schaim
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
High Energy ◽  
Muon Spectrum

The rate of energy loss of high-energy cosmic ray muons

1963 ◽  
Vol 275 (1362) ◽  
pp. 391-410 ◽  
Keyword(s):  
Energy Spectrum ◽  
Energy Loss ◽  
Sea Level ◽  
Cosmic Ray ◽  
Nuclear Interaction ◽  
High Energy ◽  
Level Energy ◽  
Muon Spectrum ◽  
The Third ◽  
Muon Mass

The rate of energy loss of muons is examined by com paring the observed depth-intensity relation with that predicted from a knowledge of the sea-level energy spectrum of cosmic ray muons. The evidence for each of the parameters entering into the analysis is assessed and estimates are made of the sea-level muon spectrum up to 10000 GeV and the depth-intensity relation down to 7000 m.w.e. The effect of range-straggling on the underground intensities is considered and shown to be important at depths below 1000 m.w.e. Following previous workers the energy loss relation is written as -d E /d x =1.88+0.077 in E ' m / mc 2 + b E MeV g -1 cm 2 , where E ' m is the maximum transferrable energy in a /i-e collision and m is the muon mass. The first two terms give the contribution from ionization (and excitation) loss and the third term is the combined contribution from pair production, bremsstrahlung and nuclear interaction. The best estimate of the coefficient b from the present work is b = (3.95 + 0.25) x 10 -6 g -1 cm 2 over the energy range 500 to 10000 GeV, which is close to the theoretical value of 4.0 x 10 -6 g -1 cm 2 . It is concluded that there is no evidence for any marked anomaly in the energy loss processes for muons of energies up to 10000 GeV.

Estimating of Cherenkov Radiation in Extensive Air Showers Using CORSIKA Code for Tunka133 EAS Cherenkov Array

2015 ◽  
Vol 754-755 ◽  
pp. 807-811
Author(s):  
A.A. Al-Rubaiee ◽  
Uda Hashim ◽  
Mohd Khairuddin Md Arshad ◽  
A. Rahim Ruslinda ◽  
R.M. Ayub ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Energy Range ◽  
Cosmic Ray ◽  
High Energy ◽  
Extensive Air Showers ◽  
Cherenkov Light ◽  
Mass Composition ◽  
Air Showers ◽  
Good Ability ◽  
The Given

The simulation of Cherenkov light Lateral distribution function (LDF) in Extensive Air Showers (EAS) initiated primary particles such as primary calcium, argon, proton iron nuclei, neutron and nitrogen have been performed using CORSIKA program for conditions and configurations of Tunka133 EAS Cherenkov array. The simulation was fulfilled at the high energy range 1014-1016eV for four different zenith angles 0o, 10o, 15oand 30o. The results of the simulated Cherenkov light LDF are compared with the measurements of Tunka133 EAS array for the same particles and energy range mentioned above. This comparison may give the good ability to reconstruct the energy spectrum and mass composition of the primary cosmic ray particles in EAS. The main feature of the given approach consists of the possibility to make a library of Cherenkov light LDF samples which could be utilized for analysis of real events which can be detected with different EAS arrays and reconstruction of the primary cosmic rays energy spectrum and mass composition of EAS particles.

Tokyo large air shower project

1968 ◽  
Vol 46 (10) ◽  
pp. S255-S258 ◽  
Author(s):  
T. Matano ◽  
M. Nagano ◽  
K. Suga ◽  
G. Tanahashi
Keyword(s):  
Energy Spectrum ◽  
Particle Density ◽  
Cosmic Ray ◽  
High Energy ◽  
Size Spectrum ◽  
Telemetry System ◽  
Simple Experiment ◽  
Air Showers ◽  
Fundamental Idea ◽  
Air Shower

A preliminary experiment to detect large air showers by means of radio echoes and to study the high-energy end of the primary cosmic-ray energy spectrum has been started at this Institute. The fundamental idea and the first approach of the experiment are presented. Using the telemetry system between two pairs of a simple scintillation array, which has been constructed to identify and calibrate the showers in the above experiment, the decoherence curve of air showers has been measured between 100 and 1 300 m together with the particle density in each detector. This simple experiment will give the power of the size spectrum above 109.

scholarly journals Auger-TA energy spectrum working group report

2019 ◽  
Vol 210 ◽  
pp. 01002 ◽  
Author(s):  
Tareq AbuZayyad ◽  
Olivier Deligny ◽  
Daisuke Ikeda ◽  
Dmitri Ivanov ◽  
Isabelle Lhenry-Yvon ◽  
...  
Keyword(s):  
Energy Spectrum ◽  
Attenuation Correction ◽  
Working Group ◽  
Cosmic Ray ◽  
High Energy ◽  
Energy Scale ◽  
Energy Calibration ◽  
Constant Intensity ◽  
High Energy Cosmic Rays ◽  
Surface Detector

The energy spectrum of ultra-high energy cosmic rays is the most emblematic observable for describing these particles. Beyond a few tens of EeV, the Pierre Auger Observatory and the Telescope Array, currently being exploited, provide the largest exposures ever accumulated in the Southern and Northern hemispheres to measure independently a suppression of the intensity, in a complementary way in terms of the coverage of the sky. However, the comparison of the spectra shows differences that are not reducible to an overall uncertainty on the calibration of the energy scale used to reconstruct the extensive air showers. In line with the previous editions of the UHECR workshops, a working group common to both experiments examined these differences by focusing this time on quantification of these differences in the region of the sky commonly observed, where the spectra should be in agreement within uncertainties when directional-exposure effects are taken into account. These differences are compared with the systematic uncertainties of each experiment. We have also revisited the methods of determining cosmic-ray energies and deriving the energy spectrum. We describe the surface detector (SD) spectrum obtained adopting an energy calibration based on the constant intensity cut method (CIC), a Monte Carlo-based attenuation correction, and an energy-dependent CIC attenuation correction.

A FRACTAL-DISCRETE SCHEME FOR COSMIC PARTICLE ACCELERATION

2007 ◽  
Vol 16 (02n03) ◽  
pp. 521-526
Author(s):  
A. L. DOS SANTOS ◽  
L. P. L. DE OLIVEIRA ◽  
B. E. J. BODMANN ◽  
M. T. VILHENA
Keyword(s):  
Particle Acceleration ◽  
Energy Spectrum ◽  
Energy Range ◽  
Power Law ◽  
Cosmic Ray ◽  
High Energy ◽  
Cosmic Particle ◽  
Observational Fact ◽  
Very High Energy ◽  
Very High

The present article is an attempt to provide a parametrization for particle acceleration probabilities in the very high energy range combining a discrete fractal scheme for interaction probabilities and the observational fact of a power law energy spectrum for cosmic ray particles.

scholarly journals HIGH ENERGY COSMIC RAYS, GAMMA RAYS AND NEUTRINOS FROM AGN

2008 ◽  
Vol 23 (24) ◽  
pp. 1991-1997 ◽  
Author(s):  
YUKIO TOMOZAWA
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
Active Galactic Nuclei ◽  
Gamma Rays ◽  
Heavy Particle ◽  
Galactic Nuclei ◽  
Cosmic Ray ◽  
High Energy ◽  
Neutrino Detectors ◽  
High Energy Cosmic Rays

The author reviews a model for the emission of high energy cosmic rays, gamma-rays and neutrinos from AGN (Active Galactic Nuclei) that he has proposed since 1985. Further discussion of the knee energy phenomenon of the cosmic ray energy spectrum requires the existence of a heavy particle with mass in the knee energy range. A possible method of detecting such a particle in the Pierre Auger Project is suggested. Also presented is a relation between the spectra of neutrinos and gamma-rays emitted from AGN. This relation can be tested by high energy neutrino detectors such as ICECUBE, the Mediterranean Sea Detector and possibly by the Pierre Auger Project.

Energy spectrum of cosmic ray primaries at super high energies estimated from the recent balloon-borne calorimeter measurements

1983 ◽  
Vol 61 (3) ◽  
pp. 434-439 ◽  
Author(s):  
D. P. Bhattacharyya
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
High Energy ◽  
Japanese American ◽  
Primary Spectrum ◽  
Atmospheric Diffusion ◽  
Neutron Spectra ◽  
High Energy Cosmic Rays ◽  
High Energies ◽  
Scaling Hypothesis

The energy spectrum of primary cosmic ray particles has been estimated from the analysis of the chemical composition data of high energy cosmic rays, data obtained by the Japanese American cooperative emulsion experiments for proton and helium intensities and the Goddard Space Flight Centre measurements for cosmic ray nuclei. The results indicate no drastic change in abundance ratios at high energies. The elemental fluxes have been calculated by assuming that the primary cosmic ray nuclei break up into their constituent nucleons near the top of the atmosphere. The calculated total primary spectrum in the range 2–300 TeV follows the form N(E) dE = 2.24 × 104 E−2.7 dE where E is the energy expressed in GeV/nucleon and N(E) is the intensity expressed in (m2∙s∙sr∙GeV/nucleon) −1.Using this primary spectrum as the source of nucleons near the top of the atmosphere, the sea level proton and neutron spectra have been estimated by using the Feynman scaling hypothesis and the conventional nucleon-atmospheric diffusion equation. The derived spectra are in accord with the measured proton and neutron spectra of Brooke and Wolfendale, Ashton and Coates, and Ashton et al.

scholarly journals Cosmic-Ray Energy Spectrum and High-Energy Particles in Supernova

1963 ◽  
Vol 30 (6) ◽  
pp. 804-815 ◽  
Author(s):  
Humitaka Satô
Keyword(s):  
Energy Spectrum ◽  
Cosmic Ray ◽  
High Energy ◽  
High Energy Particles
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