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.

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]

scholarly journals Fieldable Muon Spectrometer Using Multi-Layer Pressurized Gas Cherenkov Radiators and Its Applications

2021 ◽  
Author(s):  
Junghyun Bae ◽  
Stylianos Chatzidakis
Keyword(s):  
Precise Measurement ◽  
High Spatial Resolution ◽  
Cosmic Ray ◽  
High Accuracy ◽  
Muon Spectrum ◽  
Momentum Range ◽  
Detector Arrays ◽  
Muon Spectrometer ◽  
Conventional Radiation ◽  
Muon Momentum

Abstract Cosmic ray muons have been considered as a non-conventional radiation probe in various applications. To utilize cosmic ray muons in engineering applications, two important quantities, trajectory and momentum, must be known. The muon trajectories are easily reconstructed using two-fold detector arrays with a high spatial resolution. However, precise measurement of muon momentum is difficult to be achieved without deploying large and expensive spectrometers such as solenoid magnets. Here, we propose a new method to estimate muon momentum using multi-layer pressurized gas Cherenkov radiators. This is accurate, portable, compact (< 1m3), and easily coupled with existing muon detectors without the need of bulky magnetic or time-of-flight spectrometers. The results show that not only our new muon spectrometer can measure muon momentum with a resolution of ±0.5 GeV/c in a momentum range of 0.1 to 10.0 GeV/c, but also we can reconstruct cosmic muon spectrum with high accuracy (~90%).

scholarly journals Effect of Solar Modulation on the Low Energy Sea Level Muon Spectrum Near the Geomagnetic Equator

1978 ◽  
Vol 31 (5) ◽  
pp. 451 ◽  
Author(s):  
DP Bhattacharyya
Keyword(s):  
Experimental Data ◽  
Sea Level ◽  
Low Energy ◽  
Solar Modulation ◽  
Recent Experimental Data ◽  
Geomagnetic Equator ◽  
Muon Spectrum ◽  
Muon Intensity ◽  
Theoretical Results

A study is made of the influence of long-term solar modulation on the low energy sea level muon spectrum near the geomagnetic equator. Recent experimental data are compared with theoretical results calculated from the phenomenological model of Allkofer and Dau. It is suggested that the observed enhancement in the muon intensity is mainly due to a shift in the solar potential.

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 cosmic ray spectra at large zenith angles

1961 ◽  
Vol 265 (1320) ◽  
pp. 117-132 ◽  
Keyword(s):  
Sea Level ◽  
Meson Production ◽  
Cosmic Ray ◽  
Great Accuracy ◽  
Statistical Fluctuation ◽  
Momentum Range ◽  
Production Spectrum ◽  
A Value ◽  
The Mean ◽  
Particle Intensity

Measurements have been made at Durham (200ft. above sea level) with an emulsion spectrograph of the absolute cosmic ray particle intensity in the momentum range 1 to 100 GeV/ c at zenith angles of between 65° and 85°. It is found that a differential π-meson production spectrum of the form I 0 E -y fits closely the present results as well as the accepted vertical spectrum. The values of the parameters when E lies between 6 and 1000 GeV are given by the equations I 0 = 0.425 — 01.25 log 10 E and y = 3.92 — 0.944 (1 — 0.125 log 10 E ) -1 and their approximate constant values in this range are 0T5 and 2*55 respectively. The analysis is based on the model of Barrett, Bollinger, Cocconi, Eisenberg & Greisen (1952) but, in addition, the effects of scattering and geomagnetic deflexion of u-mesons in the atmosphere have been taken into account as well as their production over a range of atmospheric depths. Although in principle it should be possible from the form of the sea-level spectra at large zenith angles to determine the relative numbers of π- and K -mesons at production, it is shown that very great accuracy is required in order to do so. Nevertheless, the agreement between the theoretical curves and the experimental measurements indicates that the main assumptions concerning the production and propagation of mesons in the atmosphere are correct. The mean positive to negative ratio is 1.39±0.08, a value rather larger than is found by other observers at 68°, but within statistical fluctuation.

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