Atmospheric Effects on Cosmic-Ray Intensity Near Sea Level

1953 ◽  
Vol 92 (2) ◽  
pp. 454-461 ◽  
Author(s):  
S. Olbert
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Atmospheric Effects ◽  
Cosmic Ray Intensity

ATMOSPHERIC EFFECTS ON COSMIC RAY INTENSITY AT SEA LEVEL

1959 ◽  
Vol 37 (2) ◽  
pp. 85-101 ◽  
Author(s):  
P. M. Mathews
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Barometric Pressure ◽  
Theoretical Formula ◽  
Atmospheric Effects ◽  
Cosmic Ray Intensity ◽  
Statistical Fluctuations ◽  
Nucleonic Component ◽  
Primary Origin ◽  
First Time

Cosmic ray intensity variations of primary origin and those caused by meteorological changes appear superposed in records obtained from meson counter telescopes and neutron monitors at sea level. The study of either of these types of variation is thus greatly complicated by the presence of the other. In the present work, we have for the first time taken the step of processing the raw data to eliminate primary variations (and the inherent statistical fluctuations) so as to make possible a direct comparison of the remaining variations with the changes in atmospheric variables over the same period. The subsequent analysis confirms the expectation that there are no appreciable atmospheric effects on the intensity of the nucleonic component beyond the well-known effect associated with the sea level barometric pressure B. But in the meson case there is strong evidence that the widely used set of variables H100, T100 (the height and temperature of the 100-mb level) and B is not very suitable for representing atmospheric effects; it seems essential to include a variable representing temperatures in the lower part of the atmosphere, and the set of variables T800 (temperature of the 800-mb layer), H100, and B, with coefficients kT = −.082 ±.008%/°C, kH = −3.04 ±.61%/km, and kB = −.134 ±.004%/mb appears to be the best. The theoretical formula of Dorman (1957), with a barometric coefficient β = −.147 ±.004%/mb and with the term representing the "temperature effect" reduced by a factor.76 ± .03, gives slightly better results. However, the improvement, at least in the case of the data we have analyzed, is too small to justify the great labor involved in using this formula.

scholarly journals 40. Separation of extra terrestrial variations in cosmic ray intensity and atmospheric effects by differential measurements by G–M telescopes

1958 ◽  
Vol 6 ◽  
pp. 386-391
Author(s):  
E. A. Brunberg
Keyword(s):  
Daily Variation ◽  
Cosmic Ray ◽  
The Other ◽  
Atmospheric Effects ◽  
Cosmic Ray Intensity ◽  
Difference Of Opinion

The daily variation of cosmic ray intensity can arise partly from atmospheric and partly from non-atmospheric effects. There is at present a difference of opinion whether this latter effect is completely due to extra terrestrial causes or not.The purpose of the present paper is to suggest a method by which the atmospheric effects could be separated from the other variations without any assumptions about the mechanism of the atmospheric influence.

RESPONSE OF MU-MESON DETECTORS DEEP IN THE ATMOSPHERE TO PRIMARY COSMIC-RAY PARTICLES OF MAGNETIC RIGIDITY BETWEEN 10 AND 25 GV

1967 ◽  
Vol 45 (5) ◽  
pp. 1643-1653 ◽  
Author(s):  
T. Mathews ◽  
G. G. Sivjee
Keyword(s):  
Sea Level ◽  
Scintillation Counter ◽  
Cosmic Ray ◽  
Decay Rates ◽  
Atmospheric Effects ◽  
Ionization Chambers ◽  
Corrected Data ◽  
Counter Telescope ◽  
East West ◽  
Different Altitudes

The cosmic-ray mu-meson intensities at three different altitudes at the equator were measured as a function of zenith and azimuth angles by means of a portable scintillation counter telescope of semi-opening angles 23°. The data were analyzed to assess the effects of differences in pi- and mu-meson decay rates on the intensity of the penetrating ionizing component at different zenith angles. It was found that the changes of intensity as a function of zenith angles could be attributed almost entirely to differences in atmospheric absorption, provided that at all zenith angles the threshold rigidities were the same. Hence the intensities measured at different zenith angles in the east–west plane at the equator could be corrected to remove the atmospheric effects and the corrected data used for determining the response of meson detectors at sea level to particles of rigidity up to 25 GV. The response curve thus obtained is presented and compared with that obtained from sea-level latitude surveys by means of ionization chambers.

Cosmic-Ray Intensity Fluctuations at Sea Level

1954 ◽  
Vol 96 (4) ◽  
pp. 1116-1123 ◽  
Author(s):  
Robert L. Chasson
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Intensity Fluctuations

Sea level cosmic ray intensity and threshold rigidity

Tellus ◽  
1963 ◽  
Vol 15 (2) ◽  
pp. 184-193 ◽  
Author(s):  
ARNE ELD SANDSTRÖM ◽  
MARTIN A. POMERANTZ ◽  
BENGT-OLOV GRÖNKVIST
Keyword(s):  
Sea Level ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

COSMIC-RAY INTENSITY VARIATIONS AT SEA LEVEL DURING MAGNETIC-STORM PERIODS

1958 ◽  
Vol 36 (5) ◽  
pp. 635-637 ◽  
Author(s):  
G. Ramaswamy ◽  
S. D. Chatterjee
Keyword(s):  
Sea Level ◽  
Magnetic Storm ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity
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