High-Energy Protons in Nuclear Interaction of 220-Mevπ−Mesons in Nuclear Emulsions

1954 ◽  
Vol 93 (4) ◽  
pp. 848-850 ◽  
Author(s):  
Gyo Takeda
Keyword(s):  
Nuclear Interaction ◽  
High Energy ◽  
Nuclear Emulsions

On the Nuclear Interaction ofπ−Mesons in Nuclear Emulsions

1951 ◽  
Vol 82 (1) ◽  
pp. 105-106 ◽  
Author(s):  
G. Bernardini ◽  
E. T. Booth ◽  
L. Lederman ◽  
J. Tinlot
Keyword(s):  
Nuclear Interaction ◽  
Nuclear Emulsions

Solar neutron flux in the energy range 20–160 MeV

1970 ◽  
Vol 48 (18) ◽  
pp. 2155-2161 ◽  
Author(s):  
C. Y. Kim
Keyword(s):  
Neutron Flux ◽  
Energy Range ◽  
Sunspot Number ◽  
Solar Flares ◽  
Energy Region ◽  
High Energy ◽  
The Sun ◽  
Solar Neutron ◽  
Nuclear Emulsions ◽  
The Difference

An attempt to measure the flux of high-energy solar neutrons was made by measuring the difference in flux from the direction of the sun and from the symmetrical direction about the zenith, using oriented nuclear emulsions flown by balloon on July 30, 1966 from Fort Churchill, Manitoba.An excess of (2.2 ± 2.5) × 10−2 neutrons cm−2 s−1 was observed from the direction of the sun in the energy region of 20–160 MeV. On the day of the flight the sunspot number was 63, and no major solar flares were reported.

scholarly journals Observation of charmed particles produced by high-energy photons in nuclear emulsions coupled with a magnetic spectrometer

1981 ◽  
Author(s):  
B. Conforto ◽  
A. S Conti ◽  
M. m. Chernyavski ◽  
M. G. Dagliana ◽  
M. Dameri ◽  
...  
Keyword(s):  
High Energy ◽  
Magnetic Spectrometer ◽  
Nuclear Emulsions

Horizontal air showers induced by muons with energy above 1013 eV

1968 ◽  
Vol 46 (10) ◽  
pp. S369-S372 ◽  
Author(s):  
T. Matano ◽  
M. Nagano ◽  
S. Shibata ◽  
K. Suga ◽  
G. Tanahashi ◽  
...  
Keyword(s):  
Size Distribution ◽  
Zenith Angle ◽  
Nuclear Interaction ◽  
High Energy ◽  
Cloud Chamber ◽  
The Other ◽  
Active Particle ◽  
Air Showers ◽  
Experimental Distribution ◽  
Electromagnetic Showers

We have been observing horizontal air showers to study the high-energy interactions of muons. Nine horizontal air showers of size greater than 104 and zenith angle above 70° were observed. Two of these showers showed evidence that they are not pure electromagnetic showers but nucleonic showers. One shower contained a nuclear-active particle which produced a nuclear interaction in the cloud chamber, and the other shower contained a muon which penetrated about 103 g cm−2 of iron absorber. The size distribution of the horizontal showers was compared with the calculated one assuming that the nuclear interaction of high-energy muons was negligible. The discrepancy between the experimental distribution and the calculated one is reduced if the nuclear interaction of high-energy muons is taken into account, which supports our view that the horizontal air showers (at least some fraction of them) are produced by nuclear interactions of high-energy muons.

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.

High Energy Cosmic-Ray Showers in Nuclear Emulsions

1951 ◽  
Vol 81 (2) ◽  
pp. 239-244 ◽  
Author(s):  
L. S. Osborne
Keyword(s):  
Cosmic Ray ◽  
High Energy ◽  
Nuclear Emulsions

Anomalous fractal dimension and Ginzburg–Landau phase transition study in high energy nuclear interaction

2012 ◽  
Vol 45 (2) ◽  
pp. 181-187 ◽  
Author(s):  
Dipak Ghosh ◽  
Argha Deb ◽  
Ruma Saha ◽  
Rupa Das ◽  
Nurul Alam
Keyword(s):  
Phase Transition ◽  
Fractal Dimension ◽  
Nuclear Interaction ◽  
High Energy ◽  
Ginzburg Landau ◽  
Transition Study
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