A Preliminary Directional Study of Cosmic Rays at High Altitude. II. Experimental Results and Interpretation

Winckler, J. R.; Stroud, W. G.; Shanley, T. J. B.

doi:10.1103/physrev.76.1012

Cited by 14 publications

(3 citation statements)

References 6 publications

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“…Winckler and co-workers 23 found the value (0.23=b0.01)/cm 2 sec sterad for the total vertical flux under 1.9 cm Pb at 56°. Van Allen and Singer 24 found the value 0.29±0.03 above the atmosphere at 58°.…”

Section: Flux Of Primary Alpha Particlesmentioning

confidence: 93%

Measurement of Multiply Charged Cosmic Rays by a New Technique

Linsley

1955

Phys. Rev.

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The Cerenkov effect has been applied to the problem of determining the charge of cosmic rays. Cloud chamber photographs have been obtained of the events that caused large signals from a thin Cerenkov counter during a balloon flight which carried the apparatus above most of the atmosphere. They show that the Cerenkov counter was notably effective at discriminating against the background effects that plague counter measurements on the charge spectrum of cosmic rays, for a relatively large proportion of the signals were caused by single heavily ionizing particles. The theory of the Cerenkov effect associates a lower velocity limit with the signal amplitude requirement that those particles met. Their ionization was determined well enough to classify particles of such velocity as having Z~2 or Z>2 with considerable certainty. The vertical flux of doubly charged particles with kinetic energy > (610±100) Mev/nucleon beneath 17 g/cm 2 of atmosphere and 13 g/cm 2 of local matter is found to be (79dbll)/ m 2 sec steradian. That result and currently accepted assumptions concerning absorption imply the value (135±20)/m 2 sec steradian for the extrapolated vertical flux of primary alpha particles with energy above (670=bl00) Mev/nucleon. Some of the alpha particles were seen to interact in copper plates within the cloud chamber. The observations indicate that the collision mean free path is (100±25) g/cm 2 . The problem of counter measurements on components heavier than helium is scrutinized.

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Section: Flux Of Primary Alpha Particlesmentioning

confidence: 93%

Measurement of Multiply Charged Cosmic Rays by a New Technique

Linsley

1955

Phys. Rev.

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“…We use the model d = d v .P(9), valid at all zenith angles. The form of P(6), as proposed by Winckler and Stroud (1949), can be derived using a standard atmospheric model for pressure o(r) = e<,exp[ -ar] as: where 8 = r-r e ,r e is the sea-level Earth radius at the telescope site and is a function of the geographic latitude of the station, r 0 -r e is the altitude of the telescope site, and a' 1 is the scaleheight of the atmosphere and equals 0.12 when b,r e and r 0 are measured in kilometres. Winckler and Stroud used the correction factor ' l ( ' ) i 0 7 ( r 0 / 2 ) cos 2 0 + 6 which is the expression for P(6) when r 0 = r e and second order terms in 5 are neglected.…”

Section: Calculating the Coupling Coefficientsmentioning

confidence: 99%

Extensions to the Coupling Coefficient Calculations for Muon Telescopes

Baker

Duldig

Humble

1989

Publ. Astron. Soc. Aust.

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The calculation of coupling coefficients for muon telescopes has previously used interpolation from a limited set of asymptotic directions of arrival of primary particles. Furthermore, these calculations have not incorporated curvature of the atmosphere and thus diverge from the true response at zenith angles greater than about 75 degrees. The necessary extensions to calculate coupling coefficients at arbitrary zenith angles are given, including an improved method of incorporating the asymptotic directions of the primary particles. It is shown, using this method, that certain coupling coefficients are highly sensitive to small changes in asymptotic directions for some telescope configurations.

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“…Atmospheric absorber depths (Winkler and Stroud 1949) and ice absorber depths were calculated for all possible counter pairs Proc.ASA6W 1985 (one counter in each wall) for a range of telescope depths in the ice. Optimization of the system depth was then achieved by firstly calculating the differential count rate response (Cooke 1975) for all the counter pairs described above and summing these to obtain several integrated responses, for various zenith angle ranges, at each system depth..…”

Section: Telescope Design and Optimizationmentioning

confidence: 99%

A Medium Rigidity Muon Experiment for the South Pole Station

Duldig¹,

Jacklyn²,

Pomerantz

1985

Publ. Astron. Soc. Aust.

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A proposal for a medium rigidity muon telescope system to be installed at the U.S. South Pole Station for observations of time variations of cosmic ray intensity is at present being prepared by Professor Pomerantz, Director of the Bartol Research Foundation, University of Delaware and Drs Jacklyn and Duldig of the Cosmic Ray Section, Antarctic Division, Department of Science. A novel approach to medium energy cosmic ray observations viewing in equatorial to mid-latitude directions is described. The absorber depth required for the proposed 50-1000 GV rigidity range would be achieved by locating the telescope system at a depth of approximately 7 metres water equivalent (MWE) in the ice and viewing at high zenith angles. Optimization techniques used in the telescope design are presented together with the unique advantages of the location. Justification for the experiment and comparison with important observatories in this rigidity range are also discussed.

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A Preliminary Directional Study of Cosmic Rays at High Altitude. II. Experimental Results and Interpretation

Cited by 14 publications

References 6 publications

Measurement of Multiply Charged Cosmic Rays by a New Technique

Measurement of Multiply Charged Cosmic Rays by a New Technique

Extensions to the Coupling Coefficient Calculations for Muon Telescopes

A Medium Rigidity Muon Experiment for the South Pole Station

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