Der Tagesgang der kosmischen Ultrastrahlung II

1956 ◽  
Vol 11 (7) ◽  
pp. 556-561
Author(s):  
E. Remy ◽  
A. Sittkus
Keyword(s):  
Cosmic Rays ◽  
Diurnal Variation ◽  
Zenith Angle ◽  
Cosmic Ray ◽  
Center Of Gravity ◽  
Cosmic Ray Intensity ◽  
Recurrence Tendency

The total cosmic-ray intensity was measured in 1953 near Freiburg i. Br. (48° N, 8° E, 1200 m) by a countertelescope in three different ranges of zenith-angle (center of gravity 10°, 20°, 30°). The behavior of inclined radiation with the center of gravity at 40° can be deduced from these measurements by calculation. From the examination of the diurnal variation, obtained by averaging over three days only, the following factors can be seen:1. There are often several maxima and minima during one day. The time, the height, and the number of maxima change from day to day.2. A correlation with earthmagnetic disturbances with 27-day-recurrence-tendency is indicated.3. The diurnal variation of cosmic-rays coming near the vertical differs strongly from those coming from inclined directions. The dependence of zenith-angle is variable.

Two anisotropies of the cosmic-ray particles producing the cosmic-ray diurnal variation

1968 ◽  
Vol 46 (10) ◽  
pp. S828-S830
Author(s):  
Masatoshi Kitamura
Keyword(s):  
Cosmic Rays ◽  
Diurnal Variation ◽  
Interplanetary Space ◽  
Geomagnetic Latitude ◽  
Cosmic Ray ◽  
Diurnal Variations ◽  
Low Energy ◽  
The Other ◽  
Energy Spectra ◽  
Cosmic Ray Intensity

The solar diurnal variations of both meson and nucleon components of cosmic rays at sea level at geomagnetic latitude 57.5° and geomagnetic longitude 0° are analyzed by the model in which two anisotropies of cosmic-ray particles (one of them, Δj1, from about 20 h L.T. and the other, Δj2, from about 8 h L.T. in interplanetary space) produce the solar diurnal variation of the cosmic-ray intensity on the earth.When the energy spectra of Δj1 and Δj2 are represented by [Formula: see text] and [Formula: see text], respectively, where j0(E) is the normal energy spectrum of the primary cosmic rays, it is shown that the evaluation for m1 = 1, 2, m2 = 0 and the cutoffs at 8 and 10 BeV on the low-energy side of spectra of both Δj1 and Δj2 agree well with the observational results at Deep River.

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

The results of simultaneous measurements of the cosmic-ray intensity over the Antarctic and Arctic

1968 ◽  
Vol 46 (10) ◽  
pp. S823-S824
Author(s):  
S. N. Vernov ◽  
A. N. Charakhchyan ◽  
T. N. Charakhchyan ◽  
Yu. J. Stozhkov
Keyword(s):  
Cosmic Rays ◽  
Temperature Effects ◽  
Cosmic Ray ◽  
Primary Component ◽  
Low Energy ◽  
Cosmic Ray Intensity ◽  
Simultaneous Measurements ◽  
Murmansk Region ◽  
The Antarctic

The results of the analysis of data obtained from measurements carried out by means of regular stratospheric launchings of cosmic-ray radiosondes over the Murmansk region and the Antarctic observatory in Mirny in 1963–66 are presented. The problem of the anisotropy of the primary component of low-energy cosmic rays and of temperature effects on the cosmic-ray intensity in the atmosphere are discussed.

scholarly journals 36. The 27-day variation in cosmic ray intensity and in geomagnetic activity

1958 ◽  
Vol 6 ◽  
pp. 332-344 ◽  
Author(s):  
Scott E. Forbush
Keyword(s):  
Harmonic Analysis ◽  
Geomagnetic Activity ◽  
Statistical Significance ◽  
Cosmic Ray ◽  
Magnetic Activity ◽  
Effective Number ◽  
Cosmic Ray Intensity ◽  
Fourth Group ◽  
Sunspot Minimum ◽  
Recurrence Tendency

The amplitude of the average 27-day wave in cosmic ray intensity, at Huancayo, Peru, and its phase relative to that for the 27-day wave in international magnetic character figure (ICF) is determined from results of harmonic analysis of data for each of 246 intervals (or solar rotations) of 27 days. From these data, the variability of which is essential for tests of statistical significance, the amplitude of the average 27-day wave in cosmic ray intensity and its phase relative to that in geomagnetic activity is determined for each of three groups of solar rotations selected according to the average of the amplitudes of the 27-day waves in magnetic activity. A fourth group contained only 27-day intervals in which large cosmic ray decreases occurred. Relative to that in magnetic activity, the phase of the 27-day wave in cosmic ray intensity is found for the averages, to be the same for the four groups.The maxima of the average cosmic ray waves occur about 1·5 days after the minima of the corresponding waves in ICF. In general, the amplitude of the average 27-day wave in cosmic ray intensity, in the co-ordinate system in which its phase is relative to that of the 27-day wave in ICF tends to be greater for the selected groups of rotations with larger average ICF amplitudes. For most years near sunspot minimum the amplitude of the 27-day cosmic ray wave does not differ significantly from zero.Bartels found for 27-day waves in ICF the effective number of statistically independent 27-day waves for N successive solar rotations to be N/3; the number found for cosmic ray intensity is N/2. Thus, on the average the 27-day recurrence tendency is less for cosmic ray intensity than for magnetic activity.

scholarly journals Gamma Rays from Cosmic Rays

1981 ◽  
Vol 94 ◽  
pp. 309-319 ◽  
Author(s):  
A. W. Wolfendale
Keyword(s):  
Cosmic Rays ◽  
Gamma Rays ◽  
Molecular Clouds ◽  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Cosmic Ray Interactions ◽  
The Galaxy ◽  
Γ Rays ◽  
Γ Ray

It is shown that there is evidence favouring molecular clouds being sources of γ-rays, the fluxes being consistent with expectation for ambient cosmic rays interacting with the gas in the clouds for the clouds considered. An estimate is made of the fraction of the apparently diffuse γ-ray flux which comes from cosmic ray interactions in the I.S.M. as distinct from unresolved discrete sources. Finally, an examination is made of the possibility of gradients of cosmic ray intensity in the Galaxy.

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

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.

PERIODICAL FLUCTUATION STUDIES OF COSMIC-RAY DIURNAL VARIATIONS DURING THE QUIET-SUN PERIOD 1962–64

1967 ◽  
Vol 45 (8) ◽  
pp. 2733-2748 ◽  
Author(s):  
Masahiro Kodama
Keyword(s):  
Diurnal Variation ◽  
Solar Minimum ◽  
Counting Rate ◽  
Solar Rotation ◽  
Rotation Period ◽  
Cosmic Ray ◽  
Diurnal Variations ◽  
Statistical Studies ◽  
Periodic Fluctuations ◽  
Recurrence Tendency

Statistical studies of periodic fluctuations of the cosmic-ray diurnal variation have been performed, using neutron and meson component data obtained by the high-counting-rate cosmic-ray monitors at Deep River. The data cover an interval from May 1962 to October 1964, a period of descending solar activity ending near the solar minimum. It is shown that a 27-day recurrence tendency of the amplitude of the diurnal variation occasionally appears as well as shorter recurrent variations, ranging from one-half to one-sixth of the solar rotation period. The correlations of these fluctuations with some typical solar and terrestrial indices are examined in order to search for possible origins of the shorter recurrent variations. A possible connection with the Kp index exists.

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.

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