On the modulation of galactic cosmic ray intensity during solar activity cycles 19, 20, 21, 22 and early 23

2000 ◽  
Vol 27 (16) ◽  
pp. 2453-2456 ◽  
Author(s):  
James A. Van Allen
Keyword(s):  
Solar Activity ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Activity Cycles ◽  
Galactic Cosmic Ray ◽  
Solar Activity Cycles

COSMIC RAY FLUXES IN THE MAXIMUM PHASE OF SOLAR ACTIVITY CYCLES

2005 ◽  
Vol 20 (29) ◽  
pp. 6669-6671
Author(s):  
G. A. BAZILEVSKAYA ◽  
V. S. MAKHMUTOV ◽  
Y. I. STOZHKOV ◽  
A. K. SVIRZHEVSKAYA ◽  
N. S. SVIRZHEVSKY
Keyword(s):  
Solar Activity ◽  
Cosmic Rays ◽  
Cosmic Ray ◽  
Lebedev Physical Institute ◽  
Activity Maximum ◽  
Cosmic Ray Intensity ◽  
Cosmic Ray Modulation ◽  
Wide Energy ◽  
Activity Cycles ◽  
Solar Activity Cycles

The homogeneous series of primary cosmic ray intensity with energy > 100 MeV is obtained in the long-term balloon measurements of charged particle fluxes performed by Lebedev Physical Institute. Supplementing these data with those of neutron monitors enables us to study the cosmic ray modulation on the wide energy base during more than four solar activity cycles. In the periods of solar activity maximum a transition from cosmic ray decrease to recovery occurs. Changes in fluxes of cosmic rays of lower energy lag behind the changes in fluxes of cosmic rays of higher energy producing an energy hysteresis. After a while cosmic ray fluxes of all energies start to recover. In the cycles 20 and 22 the periods of transition from decline to recovery were shorter than in the cycles 21 and 23. This may be indicative of more complicated passage from the cosmic ray drift in the A > 0 conditions to the drift in the A < 0 conditions than vice versa.

scholarly journals Solar Polar Field Reversals and Secular Variation of Cosmic Ray Intensity

1980 ◽  
Vol 91 ◽  
pp. 79-86
Author(s):  
H. S. Ahluwalia
Keyword(s):  
Solar Activity ◽  
Cosmic Ray ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
Minimum Level ◽  
Solar Activity Minimum ◽  
Cosmic Ray Intensity ◽  
Activity Cycles ◽  
Solar Activity Cycles ◽  
Characteristic Manner

The profile of the well-known 11-year variation of the cosmic ray intensity appears to depend upon the emerging solar polar magnetic field regime in a very characteristic manner. During the solar activity cycle 19, the cosmic ray intensity takes about seven years to recover to its solar activity minimum level. But during the solar activity cycle 20, the recovery takes place in only about two years. It appears that these characteristic recovery modes are obtainable every other solar activity cycle. We are led to suggest two model configurations for the heliosphere. We believe that an “open” heliosphere model applies to solar activity cycles 18 and 20. A “closed” heliosphere model is obtainable during solar activity cycles 17 and 19. Our results are discussed.

scholarly journals The ‘Sterno-Etrussia’ Geomagnetic Excursion Around 2700 BP and Changes of Solar Activity, Cosmic Ray Intensity, and Climate

Radiocarbon ◽  
2004 ◽  
Vol 46 (2) ◽  
pp. 661-681 ◽  
Author(s):  
V A Dergachev ◽  
O M Raspopov ◽  
B van Geel ◽  
G I Zaitseva
Keyword(s):  
Magnetic Properties ◽  
Solar Activity ◽  
Ocean Circulation ◽  
Cosmic Ray ◽  
Thunderstorm Activity ◽  
Causal Mechanism ◽  
Global Changes ◽  
Cosmic Ray Intensity ◽  
Temperature Regimes ◽  
Galactic Cosmic Ray

The analysis of both paleo- and archeomagnetic data and magnetic properties of continental and marine sediments has shown that around 2700 BP, the geomagnetic Sterno-Etrussia excursion took place in 15 regions of the Northern Hemisphere. The study of magnetic properties of sediments of the Barents, Baltic, and White Seas demonstrates that the duration of this excursion was not more than 200–300 yr.Paleoclimatic data provide extensive evidence for a sharp global cooling around 2700 B P. The causes of natural climate variation are discussed. Changes of the galactic cosmic ray intensity may play a key role as the causal mechanism of climate change. Since the cosmic ray intensity (reflected by the cosmogenic isotope level in the earth's atmosphere) is modulated by the solar wind and by the terrestrial magnetic field, this may be an important mechanism for long-term solar climate variability. The Sterno-Etrussia excursion may have amplified the climate shift, which, in the first place, was the effect of a decline of solar activity. During excursions and inversions, the magnetic moment decreases, which leads to an increased intensity of cosmic rays penetrating the upper atmosphere. Global changes in the electromagnetic field of the earth result in sharp changes in the climate-determining factors in the atmosphere, such as temperatures, total pressure field, moisture circulation, intensity of air flows, and thunderstorm activity. In addition, significant changes in the ocean circulation patterns and temperature regimes of oceans will have taken place.

Galactic Cosmic Ray Intensity in the Upcoming Minimum of the Solar Activity Cycle

2018 ◽  
Vol 58 (2) ◽  
pp. 169-177 ◽  
Author(s):  
M. B. Krainev ◽  
G. A. Bazilevskaya ◽  
M. S. Kalinin ◽  
A. K. Svirzhevskaya ◽  
N. S. Svirzhevskii
Keyword(s):  
Solar Activity ◽  
Cosmic Ray ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
Cosmic Ray Intensity ◽  
Galactic Cosmic Ray
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