scholarly journals Sea Level Muon Spectrum and Muon Charge Ratio derived from CERN Results for Nucleon?Nucleus Inelastic Interactions

1979 ◽  
Vol 32 (4) ◽  
pp. 369 ◽  
Author(s):  
DP Bhattacharyya ◽  
RK Roychoudhury
Keyword(s):  
Sea Level ◽  
Cross Section ◽  
Pion Production ◽  
Cosmic Ray ◽  
Inelastic Collisions ◽  
Charge Ratio ◽  
Muon Spectrum ◽  
Inelastic Interactions ◽  
The Cross ◽  
Energy Moments

The sea level cosmic ray spectrum and muon charge ratio have been estimated by using the energy moments of the cross section for proton-air inelastic collisions. These energy moments have been determined by interpolation from CERN results for proton-nucleus inelastic interactions in pion production. The derived results are compared with previous work.

Das Impulsspektrum der Ultrastrahlungs-Muonen und das Ladungsverhältnis in 5200 m Höhe

1966 ◽  
Vol 21 (8) ◽  
pp. 1205-1210
Author(s):  
O. C. Allkofer ◽  
E. Kraft
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Theoretical Models ◽  
Momentum Spectrum ◽  
Charge Ratio ◽  
Lead Absorber ◽  
Muon Spectrum ◽  
Total Spectrum ◽  
Good Agreement

The momentum spectrum of cosmic ray muons and the charge ratio at 5200 m above sea level have been measured. To separate the spectrum of muons from the total spectrum a lead absorber was used. From theoretical models the spectrum of muons is calculated. Good agreement is found between the calculated and measured muon 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]

ISOSPIN DECOMPOSITION OF pp → NNππ CROSS SECTIONS — DO WE SEE A SIGN OF Δ(1600) EXCITATION IN THE nnπ+π+ CHANNEL?

2009 ◽  
Vol 24 (02n03) ◽  
pp. 450-453
Author(s):  
◽  
T. SKORODKO ◽  
M. BASHKANOV ◽  
D. BOGOSLOWSKY ◽  
H. CALÉN ◽  
...  
Keyword(s):  
Cross Section ◽  
Cross Sections ◽  
Differential Cross ◽  
Pion Production ◽  
Significant Contribution ◽  
Differential Cross Sections ◽  
Pp Collisions ◽  
Theoretical Predictions ◽  
Order Of Magnitude ◽  
The Cross

The two-pion production in pp-collisions has been investigated in exclusive measurements from threshold up to Tp = 1.36 GeV . Total and differential cross sections have been obtained for the channels pnπ+π0, ppπ+π-, ppπ0π0 and also nnπ+π+. For intermediate incident energies Tp > 1 GeV , i.e. in the region, which is beyond the Roper excitation but at the onset of ΔΔ excitation the total ppπ0π0 cross section falls behind theoretical predictions by as much as an order of magnitude near 1.2 GeV, whereas the nnπ+π+ cross section is a factor of five larger than predicted. A model-unconstrained isospin decompostion of the cross section points to a significant contribution of an isospin 3/2 resonance other than the Δ(1232). As a possible candidate the Δ(1600) is discussed.

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.

scholarly journals Quasielastic Lepton Scattering off Two-Component Dark Matter in Hypercolor Model

Symmetry ◽  
2020 ◽  
Vol 12 (5) ◽  
pp. 708 ◽  
Author(s):  
Vitaly Beylin ◽  
Maxim Bezuglov ◽  
Vladimir Kuksa ◽  
Egor Tretiakov
Keyword(s):  
Dark Matter ◽  
Total Cross Section ◽  
Cross Section ◽  
Strong Dependence ◽  
Cosmic Ray ◽  
High Energy ◽  
Dominant Contribution ◽  
Quasielastic Scattering ◽  
Two Component ◽  
The Cross

The interaction of high-energy leptons with components of Dark Matter in a hypercolor model is considered. The possibility of detection, using IceCube secondary neutrinos produced by quasielastic scattering of cosmic ray electrons off hidden mass particles, is investigated. The dominant contribution to the cross section results from diagrams with scalar exchanges. A strong dependence of the total cross section on the Dark Matter components mass is also found.

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.

On the charge ratio of cosmic-ray muons at sea level

1963 ◽  
Vol 30 (3) ◽  
pp. 762-771 ◽  
Author(s):  
P. V. Ramana Murthy
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Charge Ratio
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