Neutron monitor mass absorption coefficients at Chicago and climax during solar cycle 19 (1954-1963)

Forman, M. A.

doi:10.1029/jz070i011p02469

Cited by 9 publications

(3 citation statements)

References 11 publications

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“…While the temperature effect is generally determined by the overall profile of the atmosphere from the level of origin to the detection level, the barometric effect is determined only by the pressure at sea level. The rate of the detected cosmic ray depends on the amount of material traversed above the detector, and the barometric pressure is taken as a measure of this mass [7][8][9][10][11].…”

Section: Introductionmentioning

confidence: 99%

Influence of the Atmospheric Mass on the High Energy Cosmic Ray Muons during a Solar Cycle

Maghrabi

Alotaibi²,

Almutayri³

et al. 2015

Advances in Astronomy

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The rate of the detected cosmic ray muons depends on the atmospheric mass, height of pion production level, and temperature. Corrections for the changes in these parameters are importance to know the properties of the primary cosmic rays. In this paper, the effect of atmospheric mass, represented here by the atmospheric pressure, on the cosmic ray was studied using data from the KACST muon detector during the 2002–2012 period. The analysis was conducted by calculating the barometric coefficient (α) using regression analysis between the two parameters. The variation ofαover different time scales was investigated. The results revealed a seasonal cycle ofαwith a maximum in September and a minimum in March. Data from Adelaide muon detector were used, and different monthly variation was found. The barometric coefficient displays considerable variability at the interannual scale. Study of the annual variations ofαindicated cyclic variation with maximums between 2008 and 2009 and minimums between 2002 and 2003. This variable tendency is found to be anticorrelated with the solar activity, represented by the sunspot number. This finding was compared with the annual trend ofαfor the Adelaide muon detector for the same period of time, and a similar trend was found.

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Section: Introductionmentioning

confidence: 99%

Influence of the Atmospheric Mass on the High Energy Cosmic Ray Muons during a Solar Cycle

Maghrabi

Alotaibi²,

Almutayri³

et al. 2015

Advances in Astronomy

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“…There would be essentially no change in • at Po ~ 15 bv over the solar cycle because the total neutron intensity is changed only about 5% and •n is constant. At a station such as Climax (X --500 mm Itg), there is little or no muon contamination, and • changes by less than 3% at this cutoff rigidity (Po • 3 by), which explains the absence of a long-term change in •n [Forman, 1965].…”

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On the long-term and the altitude dependence of the barometric coefficient for neutron monitors

Lockwood¹,

Kaplan²

1967

J. Geophys. Res.

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To relate the variations in the secondary nucleonic component recorded by neutron monitors at ground elevation to the variations in the primary cosmic‐ray intensity, the effects of meteorological changes must be properly evaluated and removed from the data. Investigations have shown that the primary meteorological effect for neutron monitors arises from changes in the air mass above the neutron monitor [Simpson et al., 1953; Lockwood and Yingst, 1956; Dorman, 1957]. Insofar as the barometric pressure is a good measure of the average air mass above the station, changes of meteorological origin can then be eliminated by determining the local barometric coefficient. We should emphasize this latter point, particularly for mountain stations where perturbations from high wind speeds can be a problem [Lockwood and Calawa, 1957].

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“…An approximate quantitative cheek of the effect of water vapor on neutron monitor intensities is afforded by comparison of the barometric pressure coefficients determined for two neutron monitors at different altitudes for which approximate characteristic atmospheric water vapor contents can be determined. Comparison of the pressure coefficients reported for the Climax, Colorado, monitor [Forman, 1965] at an altitude of 3500 meters with the Denver, Colorado, monitor [Kisselbach and Chasson, 1965] has indicated that the coefficient for the Denver monitor is usually somewhat larger than that for the Climax monitor. Time variability in the difference has also been qualitatively indicated.…”

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confidence: 99%

Atmospheric water vapor and attenuation of the cosmic-ray nucleonic component

Chasson¹,

Kisselbach²,

Sharma³

1966

J. Geophys. Res.

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This communication presents some experimental results that seem to indicate that the barometric pressure coefficient customarily employed to correct terrestrial neutron monitor intensities is subject to variations in magnitude that are apparently related to changes of atmospheric water vapor content above the site of measurement. An aluminum container was placed above one section of the IGY standard neutron monitor at the University of Denver, Denver, Colorado (1600‐meter altitude, 2.93 Gv/c Quenby‐Wenk threshold). The container was filled to different depths of water for various intervals of time, and the corresponding attenuation of the nucleonic intensity was determined. Preliminary results of a statistically reliable nature have been obtained for four different water levels. The results are indicated m the table below.

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Neutron monitor mass absorption coefficients at Chicago and climax during solar cycle 19 (1954-1963)

Cited by 9 publications

References 11 publications

Influence of the Atmospheric Mass on the High Energy Cosmic Ray Muons during a Solar Cycle

Influence of the Atmospheric Mass on the High Energy Cosmic Ray Muons during a Solar Cycle

On the long-term and the altitude dependence of the barometric coefficient for neutron monitors

Atmospheric water vapor and attenuation of the cosmic-ray nucleonic component

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