Primary cosmic ray nucleon spectrum from sea-level muon spectrum and scaling hypothesis parameters

1972 ◽  
Vol 76 (1) ◽  
pp. 1-12 ◽  
Author(s):  
P. V. Ramana Murthy ◽  
A. Subramanian
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Scaling Hypothesis ◽  
Nucleon Spectrum

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]

Correlation between the sea level muon spectrum and the primary nucleon spectrum using the Cocconi–Koester–Perkins model

1979 ◽  
Vol 57 (7) ◽  
pp. 921-925 ◽  
Author(s):  
A. K. Chakrabarti ◽  
A. K. Das ◽  
A. K. De
Keyword(s):  
Sea Level ◽  
Pion Production ◽  
Spectral Shape ◽  
Muon Spectrum ◽  
Proton Proton ◽  
Absolute Value ◽  
Nucleon Spectrum ◽  
Scaling Models ◽  
The Mean ◽  
Good Agreement

Using the recent ISR data of proton–proton interactions on the inclusive production of pions and nucleons, realistic values of the mean pion inelasticity Kπ and the mean nucleon inelasticity KT have been estimated. These values have been used for the derivation of the sea level differential muon spectrum from the primary nucleon spectrum and vice versa using the CKP model as an extension of the work presented in an earlier article. It is found that none of the measured primary nucleon spectra of Ryan, Ormes, and Balasubrahmanyan and Grigorov, Rapoport, and Shestoperov fit any of the precisely measured muon spectra of Ayre, Baxendale, Hume, Nandi, Thompson, and Whalley and Allkofer, Carstensen, and Dau in spectral shape or the absolute value. On the other hand good agreement between the derived muon spectra and the spectra of Allkofer et al. and Ayre et al. is found if the primary nucleon spectra of the forms, N(Ep) = (1.38 ± 0.08)Ep−2.59 and N(Ep) = (1.00 ± 0.10)Ep−2.55, respectively, are assumed. The first form is comparable with that obtained by Brooke, Hayman, Kamiya, and Wolfendale following more approximate but similar procedure. It is also not unjustified when compared with the measured primary all nuclei spectrum of Grigorov et al. in the light of suggestions made by Ellsworth, Ito, Macfall, Siohan, Streitmatter, Tonwar, Vishwanath, Yodh, and Balasubrahmanyan. By comparing the pion production spectra derived from the same primary nucleon spectrum but using the CKP and the scaling models, it is concluded that the results are sensitive to the model assumed for the collisions.

Sea level muon spectrum from pion and kaon spectra in the atmosphere

1976 ◽  
Vol 54 (18) ◽  
pp. 1880-1883 ◽  
Author(s):  
Deba Prasad Bhattacharyya
Keyword(s):  
Diffusion Equation ◽  
Sea Level ◽  
Satellite Data ◽  
Cosmic Ray ◽  
Muon Spectrum ◽  
Momentum Range ◽  
Type Distribution ◽  
Muon Momentum ◽  
Muon Intensity

The pion and kaon spectra in the top of the atmosphere have been derived from the satellite data of cosmic ray nucleons by using the Bose-type distribution of secondary mesons produced in the inclusive reactions p + p → π− + X and p + p → K− + X. The derived pion and kaon spectra follow the relations of the form π(Eπ) dEπ = 0.184Eπ−2.6 dEπ and K(Ek) dEk = 0.036 Ek−2.6 dEk. With the help of the diffusion equation for pions and kaons in the atmosphere, the sea level muon spectrum has been derived and the results have been compared with the magnetic spectrograph data of Allkofer, Carstensen, and Dau in the muon momentum range 15–1000 GeV/c. The sea level muon intensity arising from kaon parentage increases with energy.

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.

Sea level muon spectrum derived from the Goddard Space Flight Centre measured nucleon spectrum using the Cocconi–Koester–Perkins model

1977 ◽  
Vol 55 (7-8) ◽  
pp. 629-631
Author(s):  
Kalpana Sarkar ◽  
D. P. Bhattacharyya ◽  
D. Basu
Keyword(s):  
Energy Range ◽  
Sea Level ◽  
Energy Dependence ◽  
Space Flight ◽  
Muon Spectrum ◽  
Goddard Space ◽  
Pion Energy ◽  
Nucleon Spectrum

The sea level muon spectrum is estimated from the Goddard Space Flight Centre group measured nucleon spectrum by using the model of Cocconi, Koester, and Perkins (CKP). The derived muon spectrum agrees well with the magnetic spectrograph data of Ayre, Baxendale, Hume, Nandi, Thompson, and Whalley when the energy dependence of pion inelasticity (Kπ) in the CKP model is assumed in the pion energy range 10–500 GeV. Above 50 GeV pion energy (Eπ) the pion inelasticity follows the relation Kπ = 0.1 ln Eπ.

MUON FLUXES DERIVED FROM THE DIRECTLY MEASURED PRIMARY COSMIC RAY ELEMENTAL SPECTRA

1996 ◽  
Vol 11 (30) ◽  
pp. 2427-2433
Author(s):  
MALA MITRA ◽  
PRATIBHA PAL ◽  
D.P. BHATTACHARYYA
Keyword(s):  
Cosmic Ray ◽  
Upper Atmosphere ◽  
Energy Spectra ◽  
Muon Energy ◽  
Spectral Indices ◽  
Muon Spectrum ◽  
Indirect Measurements ◽  
Large Zenith Angle ◽  
Nucleon Spectrum ◽  
The Individual

The muon energy spectra at 0° and 89° have been estimated from the decay of nonprompt and prompt mesons created by the individual elemental primary cosmic ray groups during nucleus-air collisions in the upper atmosphere and the results are found to be fairly comparable with the measured muon fluxes obtained from the direct magnetic spectrograph results in Refs. 2–4, and also from the underground indirect measurements in Refs. 5–10. The muon spectrum derived from the single slope primary nucleon spectrum with a constant spectral index of value −2.73 is only slightly different from the present result for energies below 20 TeV. The present muon spectra at large zenith angle exhibit steeper spectral indices when compared to the expected results obtained from primary elemental groups by Parente et al.

Muon sea-level intensity and primary cosmic-ray nucleon spectrum in the (1÷100) TeV energy range from the Mt. Blanc underground experiment

1983 ◽  
Vol 6 (6) ◽  
pp. 569-594 ◽  
Author(s):  
L. Bergamasco ◽  
A. Castellina ◽  
B. D'Ettorre Piazzoli ◽  
G. Mannocchi ◽  
P. Picchi ◽  
...  
Keyword(s):  
Energy Range ◽  
Sea Level ◽  
Cosmic Ray ◽  
Nucleon Spectrum ◽  
Underground Experiment

Sea level muon spectrum derived from the primary nucleon spectrum using the Cocconi–Koester–Perkins model

1979 ◽  
Vol 57 (3) ◽  
pp. 375-380
Author(s):  
A. K. Chakrabarti ◽  
A. K. Das ◽  
A. K. De
Keyword(s):  
Energy Spectrum ◽  
Sea Level ◽  
Critical Analysis ◽  
Muon Energy ◽  
Measured Spectrum ◽  
Muon Spectrum ◽  
Nucleon Spectrum ◽  
Good Agreement

In a recent paper Sarkar, Bhattacharyya, and Basu have derived the sea level muon energy spectrum from the measured nucleon spectrum of Ryan, Ormes, and Balasubrahmanyan using the Cocconi–Koester–Perkins model. They have found good agreement between this muon spectrum and the precisely measured spectrum of Ayre, Baxendale, Hume, Nandi, Thompson, and Whalley. In this report a critical analysis of the paper has been made and it is found that there are some obvious mistakes both in the formulation and in the calculation. The corrected results do not agree with the Ayre et al. spectrum. The unjustified values of some of the parameters used in their work are discussed.

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