scholarly journals The primary cosmic-ray electron spectrum in the energy range from 300 MeV to 4 BeV from 1964 to 1966

1968 ◽  
Vol 46 (10) ◽  
pp. S892-S895 ◽  
Author(s):  
Jacques L'heureux ◽  
Peter Meyer
Keyword(s):  
Energy Spectrum ◽  
Electron Spectrum ◽  
Intensity Variation ◽  
Cosmic Ray ◽  
Primary Electron ◽  
Counter Telescope ◽  
Improved Accuracy ◽  
Primary Electrons

Measurements of the primary electron spectrum were made during the summers of 1964, 1965, and 1966 using a balloon-borne counter telescope flown from Fort Churchill, Manitoba. Several balloon flights were carried out in each year in order to eliminate short-term intensity variations. This paper addresses itself to two questions: (1) the determination of the energy spectrum of primary electrons in the energy interval from 300 MeV to 4 BeV; and (2) the long-term intensity variations of the primary electron flux from 1964 through 1966. The energy spectrum was determined with improved accuracy in 1966 and agrees with our previous results. Comparison of the electron spectra obtained in 1964, 1965, and 1966 shows that, within the errors of our measurements, no long-term intensity variation existed. The upper limit for the change of flux with respect to 1965 amounts to 20% in all energy intervals studied.[Formula: see text]

Diurnal cosmic-ray variation with the inclusion of the geometrical effects and the asymptotic cones of approach

1968 ◽  
Vol 46 (10) ◽  
pp. S809-S811 ◽  
Author(s):  
L. I. Dorman ◽  
S. Fischer
Keyword(s):  
Spatial Distribution ◽  
High Latitude ◽  
Intensity Variation ◽  
Cosmic Ray ◽  
The Sun ◽  
Neutron Monitors ◽  
Asymptotic Cones ◽  
Diurnal Anisotropy ◽  
Geometrical Effects

Employing the data from cosmic-ray neutron monitors at high latitude, the spatial distribution of the axis of the diurnal anisotropy is determined. The effects of the earth's revolution around the sun on the diurnal intensity variation is investigated. A new method for further investigation of the spatial distribution of the anisotropy and for the determination of its spectra in various directions has been proposed.

scholarly journals Radiocarbon and 11-Year Variations of Cosmic Rays

Radiocarbon ◽  
1993 ◽  
Vol 35 (3) ◽  
pp. 347-350 ◽  
Author(s):  
A. A. Burchuladze ◽  
S. V. Pagava ◽  
G. I. Togonidze ◽  
M. V. Avtandilashvili
Keyword(s):  
Cosmic Rays ◽  
Cosmic Ray ◽  
Complex Problem ◽  
Short Term ◽  
The Past ◽  
Terrestrial Origin ◽  
Astrophysical Phenomena

B. P. Konstantinov and G. E. Kocharov (1965, 1967) addressed the complex problem of astrophysical phenomena and radiocarbon. Currently available data show that the determination of cosmogenic 14C in accurately dated samples of terrestrial and atmospheric origin is one of the most reliable and promising methods for studying cosmic-ray variations in the past. 14C dating samples of terrestrial origin has helped solve the problem of long-term (100 yr or more) 14C variations and, accordingly, of cosmic-ray variations in the past. Short-term (ca. 11 yr or less) variations are still under investigation (Alexeyev et al. 1971; Damon, Long and Wallick 1973).

ON THE POSSIBILITY TO SIMULTANEOUSLY DETERMINE THE LONG-TERM AVERAGE FLUXES OF SOLAR pp-NEUTRINOS AND COSMIC RAY MUONS

2011 ◽  
Vol 26 (17) ◽  
pp. 1267-1271 ◽  
Author(s):  
I. V. ANICIN ◽  
V. PEJOVIĆ ◽  
M. K. PAVIĆEVIĆ ◽  
G. AMTHAUER ◽  
B. BOEV ◽  
...  
Keyword(s):  
Stable Isotope ◽  
International Collaboration ◽  
Solar Neutrino ◽  
Neutrino Flux ◽  
Cosmic Ray ◽  
Muon Flux ◽  
Capture Reaction ◽  
Muons And Neutrinos

The Allchar mine in the southern FYR Macedonia contains the world's largest known concentration of thallium bearing minerals. LOREX (acronym for the geo-chemical LORandite EXperiment) is an international collaboration exploring the opportunity to use the rare mineral lorandite ( TlAsS 2) for the determination of the solar pp-neutrino flux, averaged over the 4.3 million year age of the deposit. Here we discuss the possibility to determine simultaneously both the solar neutrino and the cosmic ray muon flux, averaged over the same period of time. Cosmic-ray muons participate in the reaction 205 Tl (μp, n)205 Pb , whereas the neutrinos induce the capture reaction 205 Tl (νe, e)205 Pb * → 205 Pb . Both fluxes can in principle be determined by counting the number of atoms of the long-lived 205 Pb present in the mineral, produced by both muons and neutrinos in the reactions with the most abundant stable isotope, 205 Tl .

Solar modulation of galactic cosmic rays near solar minimum (1965)

1968 ◽  
Vol 46 (10) ◽  
pp. S887-S891 ◽  
Author(s):  
V. K. Balasubrahmanyan ◽  
D. E. Hagge ◽  
F. B. McDonald
Keyword(s):  
Cosmic Rays ◽  
Solar Minimum ◽  
Intensity Variation ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Solar Modulation ◽  
Time Behavior ◽  
Cosmic Ray Intensity ◽  
Radial Gradient

The results of the continuous monitoring of the intensity of cosmic rays (of energy > 50 MeV) with identical G-M counter telescopes flown in satellites IMP I, II, and III and OGO-I are presented along with the differential spectrum studies obtained from balloon flights at Fort Churchill and from satellites. A comparison of the time behavior of the G-M counter data with Deep River neutron monitor data suggests the presence of a "hysteresis" type of behavior due to spectral changes occurring near solar minimum. The existence of this "hysteresis" suggests that the radial gradient of cosmic rays near the earth could be much smaller than the ~ 10%/AU obtained by O'Gallagher and Simpson (1967) and O'Gallagher (1967) at higher energies. The long-term intensity variation of cosmic rays seems to follow the Ap index rather closely in phase, in contrast to sunspot numbers which display a pronounced phase difference with cosmic-ray intensity. The differential spectra of protons and He nuclei have been analyzed in terms of two different models for the propagation in the interplanetary medium. The modulations indicated by the present data seem to disagree with a diffusion coefficient proportional to βR where β and R are the velocity and rigidity of the particle respectively (Jokipii 1966).

Simulation of long-term cosmic-ray intensity variation

Solar Physics ◽  
1990 ◽  
Vol 125 (2) ◽  
pp. 409-414 ◽  
Author(s):  
H. Mavromichalaki ◽  
E. Marmatsouri ◽  
A. Vassilaki
Keyword(s):  
Intensity Variation ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity

scholarly journals Prediction of galactic cosmic ray intensity variation for a few (up to 10-12) years ahead on the basis of convection-diffusion and drift model

2005 ◽  
Vol 23 (9) ◽  
pp. 3003-3007 ◽  
Author(s):  
L. I. Dorman
Keyword(s):  
Interplanetary Space ◽  
Intensity Variation ◽  
Cosmic Ray ◽  
Particle Energy ◽  
Cosmic Ray Intensity ◽  
Convection Diffusion ◽  
Drift Model ◽  
Galactic Cosmic Ray ◽  
Near Future

Abstract. We determine the dimension of the Heliosphere (modulation region), radial diffusion coefficient and other parameters of convection-diffusion and drift mechanisms of cosmic ray (CR) long-term variation, depending on particle energy, the level of solar activity (SA) and general solar magnetic field. This important information we obtain on the basis of CR and SA data in the past, taking into account the theory of convection-diffusion and drift global modulation of galactic CR in the Heliosphere. By using these results and the predictions which are regularly published elsewhere of expected SA variation in the near future and prediction of next future SA cycle, we may make a prediction of the expected in the near future long-term cosmic ray intensity variation. We show that by this method we may make a prediction of the expected in the near future (up to 10-12 years, and may be more, in dependence for what period can be made definite prediction of SA) galactic cosmic ray intensity variation in the interplanetary space on different distances from the Sun, in the Earth's magnetosphere, and in the atmosphere at different altitudes and latitudes.

scholarly journals Study of the Parameters Affecting the Correlation of Background Versus Cosmic Radiation in Co2 Counters: Reliability of Dating Results

Radiocarbon ◽  
1997 ◽  
Vol 39 (3) ◽  
pp. 225-238 ◽  
Author(s):  
Yorgos Facorellis ◽  
Yannis Maniatis ◽  
Bernd Kromer
Keyword(s):  
Solar Flares ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Simple Extension ◽  
Statistical Fluctuations ◽  
Fitting Procedure ◽  
One Year ◽  
Cosmic Ray Flux

Systematic treatment of the data recorded by our guard counters and corrections introduced for meteorological factors has allowed observations on solar events clearly manifested in the readings. Examples are the solar flares of March 1989 and especially of June 1991, which caused a ca. 10% decrease in the cosmic radiation flux reaching the counters. A sinusoidal variation in the cosmic-ray flux with a period of one year is also clearly manifested in the data. The observation that the background in the 14C measurements depends on the intensity of the cosmic radiation has led to the use of monthly correlations for the determination of the best background value to be used in the age calculations. This reduces the error significantly. However, various factors such as random statistical fluctuations of the background measurements may affect the slope of the correlations and consequently the calculated age of the samples. Long-term observations of the relation between background values and coincidence counts have led to constraints in the slope of the correlation. A simple extension of the fitting procedure is explored, which maintains the physically meaningful range of the slopes, but is flexible to adjust for the seasonally varying contributions to the variations of the cosmic-ray flux.

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