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.

Pion production spectrum from primary cosmic ray spectrum and scaling constants

1977 ◽  
Vol 55 (2) ◽  
pp. 154-157 ◽  
Author(s):  
D. P. Bhattacharyya ◽  
R. K. Roy Choudhury ◽  
D. Basu
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Satellite Data ◽  
Pion Production ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Production Spectrum ◽  
Average Value ◽  
Scaling Hypothesis ◽  
Cosmic Muons

The scaling hypothesis of Dao et at. in p + p → π− + X reactions has been used to derive the sea level spectrum of cosmic muons from the satellite data of primary cosmic ray nucleons. It is found that the derived pion production spectrum depends on [Formula: see text], the average value of the Feynman variable x. Taking as input the energy spectrum of primary cosmic ray nucleons determined by Grigorov et al., as well as the sea level muon spectrum determined by Allkofer, Carstensen, and Dau, the value of [Formula: see text] at different pion energies has been estimated. A fit to the calculated results gives the following energy dependence of [Formula: see text]:[Formula: see text]

The muon energy spectrum at sea level from the intensities deep underground

1968 ◽  
Vol 46 (10) ◽  
pp. S395-S398 ◽  
Author(s):  
K. Kobayakawa
Keyword(s):  
Energy Spectrum ◽  
Energy Loss ◽  
Sea Level ◽  
Vertical Direction ◽  
Nuclear Interaction ◽  
Muon Energy ◽  
Energy Relation ◽  
Deep Underground ◽  
Energy Relations ◽  
The Average Range

The energy spectrum of muons at sea level is determined from the intensities deep underground. The following three points are different from past treatments: (1) From the energy-loss relation, −(dE/dt) = k(E) + b(E)E, including the effect of nuclear interaction and without the assumption that b is independent of E, the average range–energy relation is derived. (2) The reliable values of the factor which corrects for fluctuations in energy loss of muons passing through a great thickness of material are used. (3) Many authors measured the intensities under their respective rocks. The differences of these rocks are taken into account in the following way. The intensities are directly converted into the energy spectrum at sea level by using the appropriate average range–energy relations and correction factors. The resultant integral exponent of the energy spectrum in the vertical direction is β = 2.541 ± 0.190 with 95% confidence over the energy range 0.4–7 TeV having a weighted mean of 0.7 TeV.

scholarly journals ULTRA–HIGH-ENERGY COSMIC RAYS

2006 ◽  
Vol 21 (08n09) ◽  
pp. 1950-1961 ◽  
Author(s):  
STEFAN WESTERHOFF
Keyword(s):  
Energy Spectrum ◽  
Cosmic Rays ◽  
Energy Loss ◽  
Cosmic Ray ◽  
High Energy ◽  
Ultra High Energy ◽  
New Era ◽  
High Energy Cosmic Rays ◽  
Open Questions ◽  
The Many

One of the most striking astrophysical phenomena today is the existence of cosmic ray particles with energies in excess of 1020 eV. While their presence has been confirmed by a number of experiments, it is not clear where and how these particles are accelerated to these energies and how they travel astronomical distances without substantial energy loss. We are entering an exciting new era in cosmic ray physics, with instruments now producing data of unprecedented quality and quantity to tackle the many open questions. This paper reviews the current experimental status of cosmic ray physics and summarizes recent results on the energy spectrum and arrival directions of ultra-high-energy cosmic rays.

scholarly journals The UH-nuclei cosmic ray detector on the third high energy astronomy observatory

1981 ◽  
Vol 185 (1-3) ◽  
pp. 415-426 ◽  
Author(s):  
W.R. Binns ◽  
M.H. Israel ◽  
J. Klarmann ◽  
W.R. Scarlett ◽  
E.C. Stone ◽  
...  
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Astronomy Observatory ◽  
The Third

Energy spectrum of cosmic-ray muons at sea level

1964 ◽  
Vol 32 (6) ◽  
pp. 1524-1540 ◽  
Author(s):  
S. Miyake ◽  
V. S. Narasimham ◽  
P. V. Ramana Murthy
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Cosmic Ray

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.

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