ON DIURNAL VARIATION IN COSMIC-RAY INTENSITY AT OTTAWA

1955 ◽  
Vol 33 (10) ◽  
pp. 577-587
Author(s):  
S. D. Chatterjee ◽  
J. N. Bloom
Keyword(s):  
High Pressure ◽  
Statistical Analysis ◽  
Diurnal Variation ◽  
Ionization Chamber ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Rigorous Statistical Analysis ◽  
Local Mean ◽  
Mean Time ◽  
Barometric Coefficient

Cosmic-ray data from a high pressure integrating ionization chamber, obtained at Ottawa, for 129 complete days during September 1950 to July 1951 are subjected to rigorous statistical analysis. The barometric coefficient is −0.19% per mm. of Hg for the period covered by this analysis. The results also indicate a physically significant 24-hr. wave in cosmic-ray intensity, with an amplitude of 0.12% of the total intensity, having its maximum at about 10.40 a.m. local mean time. The existence of the semidiurnal wave, however, is not physically significant.

AN APPARENT ANOMALY OF THE BAROMETRIC COEFFICIENT FOR THE NUCLEONIC COMPONENT OF COSMIC-RAY INTENSITY

1964 ◽  
Vol 42 (10) ◽  
pp. 1847-1856
Author(s):  
S. M. Lapointe
Keyword(s):  
Statistical Analysis ◽  
Pressure Coefficient ◽  
Geomagnetic Latitude ◽  
Cosmic Ray ◽  
Attenuation Length ◽  
Cosmic Ray Intensity ◽  
Simple Theoretical Model ◽  
Standard Neutron ◽  
Nucleonic Component ◽  
Barometric Coefficient

A statistical analysis, based on three and one-half years of observational data, previously published by Lapointe and Rose (1962), produced a larger barometric coefficient for the nucleonic intensity in the standard neutron monitor at Sulphur Mountain (altitude 2283 meters) than at Ottawa (same geomagnetic latitude, sea level station).To explain this apparent anomaly, a simple theoretical model is presented which reproduces the results of this statistical analysis. The model treats the nucleonic component as consisting of two distinct cascades of nucleons, one "hard", characterized by a greater attenuation length and smaller pressure coefficient, and one "soft", characterized by a shorter attenuation length and larger pressure coefficient. The validity of the model is discussed.

Solar Magnetic Moment and Diurnal Variation in Cosmic-Ray Intensity

1954 ◽  
Vol 93 (3) ◽  
pp. 551-553 ◽  
Author(s):  
J. Firor ◽  
F. Jory ◽  
S. B. Treiman
Keyword(s):  
Diurnal Variation ◽  
Magnetic Moment ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

Note on Diurnal Variation of Cosmic-Ray Intensity

1936 ◽  
Vol 50 (9) ◽  
pp. 869-869 ◽  
Author(s):  
Julian L. Thompson
Keyword(s):  
Diurnal Variation ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

The solar semidiurnal variation of cosmic-ray intensity 70 m.w.e. underground

1968 ◽  
Vol 46 (10) ◽  
pp. S839-S843 ◽  
Author(s):  
G. Cini-Castagnoli ◽  
M. A. Dodero ◽  
L. Andreis
Keyword(s):  
Diurnal Variation ◽  
Cosmic Ray ◽  
Fermi Acceleration ◽  
Sidereal Time ◽  
Cosmic Ray Intensity ◽  
Intensity Measurements ◽  
Hourly Data ◽  
Semidiurnal Variation ◽  
Order Of Magnitude ◽  
Different Depths

Cosmic-ray intensity measurements have been carried out during the last year at a depth of 70 m.w.e. in the Monte dei Cappuccini laboratory in Torino, using solid vertical semicubical scintillator telescopes with a total area of 2 m2. Hourly data for 245 days corrected for barometric changes have been analyzed for the solar, apparent sidereal, and antisidereal daily variations whose harmonics are as follows:[Formula: see text]The true sidereal diurnal variation is estimated to have an amplitude of 0.019% with a time of maximum at 1720 h local sidereal time. The solar diurnal variation at different depths underground follows the energy dependence calculated with Axford's theory. The solar semidiurnal variation shows instead a fairly constant value at different μ energies. Its order of magnitude agrees with that expected as a result of Fermi acceleration in collisions of primaries moving in roughly solar and antisolar directions with solar wind inhomogeneities.

Pronounced diurnal variation in cosmic-ray intensity

1969 ◽  
Vol 74 (5) ◽  
pp. 1218-1229 ◽  
Author(s):  
T. Mathews ◽  
D. Venkatesan ◽  
B. G. Wilson
Keyword(s):  
Diurnal Variation ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

The Semi-Diurnal Variation in Cosmic Ray Intensity

1948 ◽  
Vol 60 (6) ◽  
pp. 509-523 ◽  
Author(s):  
Phyllis Nicolson ◽  
V Sarabhai
Keyword(s):  
Diurnal Variation ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity
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