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

THE VARIATION OF SEA LEVEL COSMIC RAY INTENSITY BETWEEN 1954 AND 1957

1958 ◽  
Vol 36 (7) ◽  
pp. 824-839 ◽  
Author(s):  
A. G. Fenton ◽  
D. C. Rose ◽  
K. B. Fenton
Keyword(s):  
Solar Activity ◽  
Sea Level ◽  
Geomagnetic Latitude ◽  
Cosmic Ray ◽  
High Solar Activity ◽  
General Level ◽  
Intensity Level ◽  
Cosmic Ray Intensity ◽  
Primary Cosmic Radiation ◽  
The One

Results from neutron monitors and meson telescopes at Ottawa (geomagnetic latitude 57° N.) and Resolute (geomagnetic latitude 83° N.) are presented for the years 1954–57, a period of increasing solar activity. The results indicate that the sea level meson intensity at these latitudes decreased by 5–6% between April 1954 and December 1957. During the same period the intensity of the nucleonic component at these stations decreased by over 22%. Investigation of the relative response of the two types of recorder to transient decreases during this period indicates that the long term change in the intensity level cannot be explained completely as an accumulation of shorter transient decreases, which become more frequent at times of high solar activity. It is concluded that the transient decreases are superimposed upon the longer term changes, each being produced by a separate modulation process but ultimately controlled by the general level of solar activity. Significant differences are found in the shape of transient decreases observed at the Canadian stations, both between different components at the one station and the same component at different stations. These may be interpreted as due to a varying energy dependence from one transient decrease to another, and to anisotropy in the primary cosmic radiation at these times.

scholarly journals Distribution of temperature coefficient density for muons in the atmosphere

2017 ◽  
Vol 3 (4) ◽  
pp. 93-102 ◽  
Author(s):  
Василий Кузьменко ◽  
Vasiliy Kuzmenko ◽  
Валерий Янчуковский ◽  
Valery Yanchukovsky
Keyword(s):  
Temperature Coefficient ◽  
Sea Level ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Temperature Coefficients ◽  
Specific Geometry ◽  
Muon Intensity

To date, several dozens of new muon detectors have been built. When studying cosmic-ray intensity variations with these detectors, located deep in the atmosphere, it is necessary to calculate all character-istics, including the distribution of temperature coeffi-cient density for muons in the atmosphere, taking into account their specific geometry. For this purpose, we calculate the density of temperature coefficients of muon intensity in the atmosphere at various zenith angles of detection at sea level and at various depths underground for different absorption ranges of primary protons and pions in the atmosphere.

Sign in / Sign up

Export Citation Format

Share Document