The High-Pressure Cloud-Chamber Cosmic-Ray Programme At La Marmolada

Nature ◽  
1955 ◽  
Vol 175 (4454) ◽  
pp. 445-448 ◽  
Author(s):  
Keyword(s):  
High Pressure ◽  
Cosmic Ray ◽  
Cloud Chamber

A High Pressure Cloud Chamber Observation of Cosmic Ray at 2740 m Elevation

1951 ◽  
Vol 6 (3) ◽  
pp. 204B-206 ◽  
Author(s):  
Y. Watase ◽  
S. Miyake ◽  
K. Suga ◽  
O. Kusumoto
Keyword(s):  
High Pressure ◽  
Cosmic Ray ◽  
Cloud Chamber

The Structure of Cosmic Ray Air Showers

1949 ◽  
Vol 2 (2) ◽  
pp. 184
Author(s):  
CBO Mohr
Keyword(s):  
High Pressure ◽  
Sea Level ◽  
Cosmic Ray ◽  
Low Density ◽  
Air Showers ◽  
Ionization Chambers ◽  
Single Chamber ◽  
Transition Effect ◽  
The Core ◽  
Rate Frequency

The structure of cosmic ray air showers at sea-level has been studied by an investigation of the burst rate frequency and the transition effect in lead, for cosmic ray bursts occurring simultaneously in two high-pressure ionization chambers with varying separation. Although extensive showers were responsible for all the coincidences observed with the larger chamber separations, they accounted for less than 3 per cent, of the bursts observed with a single chamber. Of the remaining 97 per cent., somewhat more than one-half appear to be due to nuclear disintegrations and the rest either to narrow showers of approximate radius 30 cm. or to the core of an extensive shower of low density. The extensive shower frequency was about 10 times that predicted by theory. The bearing of these results on present views of the origin and development of air showers is discussed.

A Cloud Chamber Study of the Cosmic-Ray Hard Showers

1956 ◽  
Vol 11 (1) ◽  
pp. 76-83 ◽  
Author(s):  
Saburo Miyake ◽  
Kensaku Hinotani ◽  
Kan-ichi Nunogaki
Keyword(s):  
Cosmic Ray ◽  
Cloud Chamber ◽  
Chamber Study

scholarly journals The measurement of the energy of cosmic rays I—The electro-magnet and cloud chamber

1936 ◽  
Vol 154 (883) ◽  
pp. 564-573 ◽  
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
Electric Power ◽  
Strong Magnetic Field ◽  
Heavy Water ◽  
Cosmic Ray ◽  
Cloud Chamber ◽  
Pole Piece ◽  
Actual Length ◽  
And Performance

1—The Construction and Performance of the Electro-Magnet The energy of the cosmic ray particles has been determined from the curvature of their tracks in a strong magnetic field by Kunze, and by Anderson. Kunze used a power of 500 kw in a copper solenoid weighing 1100 kg to give a magnetic field of 18,400 gauss over a chamber 16⋅4 cm in diameter. Anderson used an electro-magnet with heavy water-cooled copper coils and a relatively light iron yoke. A power of 440 kw gave a field of 15,000 gauss over a chamber 16⋅5 cm in diameter, the actual length of the tracks photographed being about 12 cm. In order to obtain a similar performance without the use of such a very large amount of electric power, an electro-magnet has been constructed of a more conventional design, that is with an iron yoke which is heavy compared with the weight of the copper coils. The iron yoke weighs about 8000 kg and the copper coils 3000 kg. Figs. 1 a and 1 b show the detail of the design, and fig. 2 shows a photograph of the magnet in use with the cloud chamber and subsidiary apparatus. The diameter of the pole face is 25 cm, and the gap can be varied from 5 to 20 cm by sliding one pole piece along the baseplate by means of a screw.

Application of Emulsion Cloud Chamber to cosmic-ray muon radiography

2015 ◽  
Vol 83 ◽  
pp. 56-58 ◽  
Author(s):  
Ryuichi Nishiyama ◽  
Seigo Miyamoto ◽  
Naotaka Naganawa
Keyword(s):  
Cosmic Ray ◽  
Cloud Chamber ◽  
Muon Radiography

EMISSION OF NUCLEI IN COSMIC RAY STARS

1950 ◽  
Vol 28a (6) ◽  
pp. 616-627 ◽  
Author(s):  
E. Pickup ◽  
L. Voyvodic
Keyword(s):  
Excited State ◽  
Energy Spectrum ◽  
Radioactive Decay ◽  
Cosmic Ray ◽  
Cloud Chamber ◽  
Photographic Emulsions ◽  
Chamber Technique ◽  
Good Agreement ◽  
Α Particles

One of the more interesting features of cosmic ray stars is that [Formula: see text] nuclei are ejected occasionally in the nuclear disintegrations. Such nuclei are characterized by the fact that, at the end of their range, they suffer radioactive decay (τ = 0.9 sec.) into [Formula: see text], which immediately splits up into two oppositely directed α-particles, giving what is usually referred to as a hammer track. In this investigation numerous examples have been observed of the emission of such nuclei in stars in photographic emulsions, the stars having from 2 to 60 prongs. In particular, it has been shown that the energy spectrum of the α-particles forming the hammer tracks is in good agreement with that observed by other workers, and also with experiments made, using the cloud chamber technique, indicating that the [Formula: see text] in this disintegration is formed in the excited state. When an electron sensitive emulsion is used it is shown that the hammer track is accompanied by the [Formula: see text] disintegration electron. The energy spectrum of the [Formula: see text] nuclei is plotted, and the mechanism of the formation is discussed for both large and small stars.

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