High-Energy Electromagnetic Phenomena in Cosmic Radiation

1955 ◽  
Vol 100 (1) ◽  
pp. 327-339 ◽  
Author(s):  
M. Koshiba ◽  
M. F. Kaplon
Keyword(s):  
Cosmic Radiation ◽  
High Energy

The HERO project for the study of high-energy primary cosmic radiation

2009 ◽  
Vol 73 (5) ◽  
pp. 593-596
Author(s):  
D. M. Podorozhnyi ◽  
E. V. Atkin ◽  
L. S. Burylov ◽  
A. G. Voronin ◽  
N. V. Kuznetsov ◽  
...  
Keyword(s):  
Cosmic Radiation ◽  
High Energy ◽  
Primary Cosmic Radiation

Detectors for cosmic particles, neutrinos and exotic matter

2020 ◽  
pp. 655-710
Author(s):  
Hermann Kolanoski ◽  
Norbert Wermes
Keyword(s):  
Dark Matter ◽  
Particle Physics ◽  
Cosmic Radiation ◽  
Charged Particles ◽  
Cosmic Ray ◽  
High Energy ◽  
Detection Methods ◽  
Astroparticle Physics ◽  
High Energy Cosmic Rays ◽  
Cosmic Origin

Astroparticle physics deals with the investigation of cosmic radiation using similar detection methods as in particle physics, however, mostly with quite different detector arrangements. In this chapter the detection principles for the different radiation types with cosmic origin are presented, this includes charged particles, gamma radiation, neutrinos and possibly existing Dark Matter. In the case of neutrinos also experiments at accelerators and reactors are included. Examples, which are typical for the different areas, are given for detectors and their properties. For cosmic ray detection apparatuses are deployed above the atmosphere with balloons or satellites or on the ground using the atmosphere as calorimeter in which high-energy cosmic rays develop showers or in underground areas including in water and ice.

scholarly journals The annihilation of fast positrons by electrons in the K-shell

1934 ◽  
Vol 146 (859) ◽  
pp. 723-736 ◽  
Keyword(s):  
Kinetic Energy ◽  
Cosmic Radiation ◽  
Nuclear Charge ◽  
Structure Constant ◽  
Photoelectric Effect ◽  
High Energy ◽  
Negative Energy ◽  
Fine Structure Constant ◽  
Quantum Process ◽  
High Energies

The probability of the simultaneous of a positron and an electron, with the emission of two quanta of radiation, has been calculated by Dirac and several other authors. From considerations of energy and momentum it follows that an electron and positron can only annihilate one another with the emission of one quantum of radiation in the presence of a third body. An electron bound in an atom could, therefore, annihilate a positron, represented by a hole on the Dirac theory, by jumping into a state of negative energy which happens to be free, the nucleus taking up the extra momentum. The process is now mathematically analogous to the photoelectric transitions to states of negative energy in the sense that the matrix elements concerned are the same, and we might expect that the effect would be most important for the electrons in the K-shell. Fermi and Uhlenbeck have calculated the process approximately, for the condition where the kinetic energy of the positron is of the order of magnitude of the ionization energy of the K-shell. The result they obtained was very small compared with the two quantum process, which is to be explained by the fact that for these small energies, the positron does not get near the nucleus. In view of the fact that positrons of energies of the order 100 mc 2 occur in considerable quantities in the showers produced by cosmic radiation, and that the primary cosmic radiation itself may consist, in part, of positrons, it becomes of interest to calculate the cross-section for the annihilation of positrons of high energy by electrons in the K-shell, and their absorption in matter, and also to compare this process with the two quantum process for high energies. In the photoelectric effect for hard γ -rays, the electron the electron leaves the atom in states of different angular momentum (described by the azimuthal quantum number l ), and the terms which give the largest contribution are roughly those for which l is of the order of the energy of the γ -ray in terms of mc 2 . For high energies, therefore, a calculation by the method of Hulme, in which the last step is carried out numerically, is out of the question, and we must find some approximate method of effecting a summation. We shall use an adaptation of Sauter's method, in which we shall treat as small the product of the fine structure constant and the nuclear charge. This method may be expected to give a good approximation for small nuclear charge. Our method has the further restriction that it is valid only when the kinetic energy of the positron is not small compared with mc 2 .

The Absorption Mean Free Path of the High-Energy Nucleonic Component of Cosmic Radiation

1953 ◽  
Vol 91 (6) ◽  
pp. 1573-1573 ◽  
Author(s):  
M. F. Kaplon ◽  
J. Z. Klose ◽  
D. M. Ritson ◽  
W. D. Walker
Keyword(s):  
Free Path ◽  
Cosmic Radiation ◽  
Mean Free Path ◽  
High Energy ◽  
Nucleonic Component

Cosmic radiation and high energy interactions

1966 ◽  
Vol 281 (4) ◽  
pp. 349-350
Author(s):  
Ricardo A.R. Palmeira
Keyword(s):  
Cosmic Radiation ◽  
High Energy

scholarly journals Nuclear disintegrations produced by cosmic rays

1949 ◽  
Vol 196 (1046) ◽  
pp. 325-343 ◽  
Keyword(s):  
Cosmic Radiation ◽  
High Energy ◽  
Energy Spectra ◽  
Angular Distributions ◽  
Excitation Energies ◽  
Wide Range ◽  
High Energy Tail ◽  
Energy And Angular Distributions ◽  
Photographic Emulsions ◽  
Α Particles

Measurements have been made on the energy and angular distributions of the charged particles from disintegration ‘stars’ produced in the silver and bromine nuclei of photographic emulsions exposed to cosmic radiation. The observations extended over a wide range of excitation energies (100 to 700 MeV). The energy spectra and angular distributions of the protons can be explained in all cases by simple evaporation theory. This energy distribution shows also a high-energy tail consisting of direct knock-on protons and slow mesons. At high excitation energies the α-particles exhibit collimation effects which are probably due to localized ‘boiling’ or a form of fission.

The Behavior of High Energy Electrons in the Cosmic Radiation

1939 ◽  
Vol 11 (3-4) ◽  
pp. 255-264 ◽  
Author(s):  
C. G. Montgomery ◽  
D. D. Montgomery
Keyword(s):  
Cosmic Radiation ◽  
High Energy ◽  
High Energy Electrons

scholarly journals An Estimate of the Flux of Free Quarks in High Energy Cosmic Radiation

1983 ◽  
Vol 36 (5) ◽  
pp. 717 ◽  
Author(s):  
CBA McCusker
Keyword(s):  
Sea Level ◽  
Cosmic Radiation ◽  
High Energy ◽  
Earth’S Crust ◽  
Calculated Concentration ◽  
Air Shower ◽  
Different Types ◽  
Earth's Crust

The flux of quarks in air shower cores at sea level is estimated from four different types of experiments. All four estimates agree and yield a quark flux of 8 x 10-12 cm-2 s- 1 sr- 1 ? The calculated concentration of quarks in the Earth's crust resulting from this flux is compared with that found in niobium in the Stanford quark search.

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