scholarly journals The Regener-Pfotzer Maximum During a Total Solar Eclipse

2021 ◽  
Vol 1 (1) ◽  
Author(s):  
Gordon McIntosh ◽  
Alaina Swanson ◽  
Liam Taylor ◽  
Erick Paul Agrimson ◽  
Kaye Smith ◽  
...  
Keyword(s):  
High Altitude ◽  
Solar Eclipse ◽  
Radiation Intensity ◽  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Total Solar Eclipse ◽  
Interaction Layer ◽  
The Earth ◽  
Cosmic Ray Flux

The Regener-Pfotzer (RP) maximum is the altitude at which cosmic radiation intensity is the greatest. A decrease of the altitude of the interaction layer, assumed to be measured by the RP maximum, has been suggested to account for a reduction in the secondary cosmic ray flux measured at the surface of the Earth during a total solar eclipse. To investigate this suggestion, high altitude cosmic radiation was measured using Geiger Mueller (GM) counters carried beneath weather balloons both before and during the total solar eclipse on 21 August 2017. The 19 and 20 August 2017 omnidirectional RP maxima occurred at an average altitude of 20.2 km ± 0.9 km. During the eclipse of 21 August 2017 the omnidirectional RP maxima occurred at an altitude of 20.4 km ± 0.8 km. The 19 and 20 August 2017 vertical coincidence RP maxima occurred at an altitude of 18.3 km ± 1.0 km. During the eclipse the vertical coincidence RP maxima occurred at 18.0 km ± 1.0 km. Our results do not show any decrease in the altitude of either the omnidirectional or the vertical coincidence RP maximum outside the range of our measurements before the eclipse.

scholarly journals Tritium and Argon-39 in Stone and Iron Meteorites

1969 ◽  
Vol 24 (2) ◽  
pp. 234-244 ◽  
Author(s):  
St. Charalambus ◽  
K. Goebel ◽  
W. Stötzel-Riezler
Keyword(s):  
Cosmic Ray ◽  
Decay Rates ◽  
Earth Atmosphere ◽  
Iron Meteorites ◽  
Production Rates ◽  
Cosmic Ray Intensity ◽  
The Earth ◽  
Cosmic Ray Flux

Tritium and argon-39 measurements of stone and iron meteorites are reported and discussed. The tritium values of stone meteorites are in general higher than those found in other laboratories. The tritium decay rates in irons were low but a relatively high tritium value was measured in the rim of the meteorites. Factors which may influence the production rates are discussed and it is concluded that the average cosmic-ray flux which irradiated the meteorites must be at least a factor of two higher than the values reported by MacDonald for the cosmic-ray intensity at the top of the earth atmosphere.

A New Determination of Muon Directional Coupling Coefficients

1968 ◽  
Vol 1 (4) ◽  
pp. 154-157
Author(s):  
D. J. Cooke ◽  
A. G. Fenton
Keyword(s):  
Cosmic Rays ◽  
Solar System ◽  
Cosmic Ray ◽  
Accurate Information ◽  
Coupling Coefficients ◽  
The Earth ◽  
Directional Coupling ◽  
Cosmic Ray Flux ◽  
Primary Cosmic Rays

Primary cosmic rays passing through the solar system carry with them valuable information about solar and astrophysical phenomena in the form of intensity and spectral variations. In order that this information be efficiently extracted from observations of the directional cosmic-ray flux at the surface of the Earth, it is essential to have accurate information available to enable the relating of the observed secondary cosmic-ray directions of motion and intensity to those outside the range of the disturbing terrestrial influences.

Cosmic ray flux at the Earth in a variable heliosphere

2008 ◽  
Vol 41 (8) ◽  
pp. 1171-1176 ◽  
Author(s):  
K. Scherer ◽  
H. Fichtner ◽  
B. Heber ◽  
S.E.S. Ferreira ◽  
M.S. Potgieter
Keyword(s):  
Cosmic Ray ◽  
The Earth ◽  
Cosmic Ray Flux

scholarly journals Calculations of temperature and barometric effects for cosmic ray flux on the Earth surface using the CORSIKA code

2013 ◽  
Vol 409 ◽  
pp. 012128 ◽  
Author(s):  
A A Kovylyaeva ◽  
A N Dmitrieva ◽  
N V Tolkacheva ◽  
E I Yakovleva
Keyword(s):  
Cosmic Ray ◽  
Earth Surface ◽  
The Earth ◽  
Cosmic Ray Flux

Cosmic-ray flux variation with height in the atmosphere

1968 ◽  
Vol 46 (10) ◽  
pp. S1020-S1022 ◽  
Author(s):  
B. S. Chow ◽  
K. K. Wu ◽  
N. Simpson ◽  
V. D. Hopper
Keyword(s):  
Cosmic Radiation ◽  
Cosmic Ray ◽  
Geiger Counter ◽  
Proton Flux ◽  
Atmospheric Depth ◽  
Altitude Range ◽  
Flux Variation ◽  
Star Production ◽  
Cosmic Ray Flux ◽  
Made In

Analysis of emulsions exposed to cosmic radiation at atmospheric depths between 10 and 40 g/cm2 at λ = 47 °S geomagnetic on 11 December 1964 shows that there is little variation with altitude in proton flux in this altitude range. However, the total star production rate increases with increasing atmospheric depth but with a smaller slope than that measured by Geiger counter. Preliminary results obtained from exposures made in November 1965 at 8.5, 28.4, and 58 g/cm2 show that the values of proton flux at 8.5 and 58 g/cm2 are lower than that at 28.4 g/cm2. A study of the rate of production of stars at λ = 43° S and 9 g/cm2 over the period April 1962 to September 1966 shows some correlation with the ground-based neutron monitor count rate. The proton flux at the top of the atmosphere at latitude 47° S is estimated as 900 ± 100 protons/m2 sr s.

The Propagation of Cosmic Radiation Through the Inter-Planetary Magnetic Field

1967 ◽  
Vol 1 (1) ◽  
pp. 29-30
Author(s):  
K. G. McCracken
Keyword(s):  
Magnetic Field ◽  
Energy Range ◽  
Cosmic Radiation ◽  
Counting Rate ◽  
Cosmic Ray ◽  
Alpha Particles ◽  
Statistical Precision ◽  
Degree Of Anisotropy ◽  
Planetary Magnetic Field ◽  
Cosmic Ray Flux

Instruments were flown on the Pioneer 6 and 7 spacecraft during 1965-66 to study the degree of anisotropy of cosmic radiation in the energy range 7.5-90 Mev/nucleón. The instruments record the cosmic ray fluxes from each of four contiguous ‘quadrants’ of azimuthal rotation of the spacecraft, for each of three energy windows 7.5-45 Mev, 45-90 Mev, and 150-350 Mev for alpha particles and heavier nuclei. In addition, the counting rate of all particles of energy >7.5 Mev is recorded, thereby providing cosmic ray data of high statistical precision useful in the study of fast changes in the cosmic ray flux.

TRANSIENT DECREASES IN COSMIC RAY INTENSITY DURING THE PERIOD OCTOBER 1956 TO JANUARY 1958

1959 ◽  
Vol 37 (5) ◽  
pp. 569-578 ◽  
Author(s):  
A. G. Fenton ◽  
D. C. Rose ◽  
K. G. McCracken ◽  
B. G. Wilson
Keyword(s):  
Forbush Decrease ◽  
Cosmic Ray ◽  
Statistical Accuracy ◽  
Short Term ◽  
Cosmic Ray Intensity ◽  
The Earth ◽  
Controlling Mechanism ◽  
Intensity Changes ◽  
Recurrence Tendency ◽  
Cosmic Ray Flux

Recent nucleon intensity data obtained from high counting rate recorders at Ottawa and Hobart, and subsidiary stations, have been examined for evidence for the superposition of transient decreases. It is concluded that, with the statistical accuracy now available due to the high counting rates, it is possible to distinguish two types of transient decreases in the observed variations, superimposed upon the slower 11-year intensity changes. One of these is an almost symmetrical event lasting up to 2 weeks and exhibiting a recurrence tendency of about 27 days, while the other is the more abrupt Forbush decrease which recovers over a period of several days. The evidence indicates that the intensity-controlling mechanism responsible for these short-term transient changes is able to influence the cosmic ray flux at the earth independently of other events that may be in progress at the time. There is also evidence that the physical process controlling the Forbush type of decrease operates over a volume large compared with the earth because the intensity changes at places as far apart as Ottawa, Canada, and Hobart, Tasmania, show changes that are the same within the accuracy of the measurements.

scholarly journals The solar eclipse and its relation with higree months

2019 ◽  
Vol 11 (22) ◽  
pp. 72-81
Author(s):  
Abdul Rahman H. S.
Keyword(s):  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
The Sun ◽  
The Moon ◽  
New Model ◽  
Earth Radius ◽  
The Earth ◽  
Equatorial Radius ◽  
Short Time

The solar eclipse occurs at short time before the crescent birth moment when the moon near any one of moon orbit nodes It is important to determine the synchronic month which is used to find Higree date. The 'rules' of eclipses are:  Y= ± 0.997  of Earth radius , the solar eclipse is central and 0.997 < |Y| < 1.026 the umbra cone touch the surface of the Earth, where Y is the least distance from the axis of the moon's shadow to the center of the Earth in units of the equatorial radius of the Earth. A new model have been designed, depend on the horizontal coordinates of the sun, moon, the distances Earth-Moon (rm), Earth-sun (rs) and |Y| to determine the date and times of total solar eclipse and the geographical coordinates of spot shadow as well as the shadow diameter and the variations with time. The results are compared with Almanac and others programs are gets a good agreements and the results show the area of eclipse shadow inversely proportional with rm /rs .The Higree month which must be begin after  the solar eclipse and the relation were discussed hear.

scholarly journals Project Apeiro - High-altitude balloon payload for measuring cosmic ray flux

2019 ◽  
Author(s):  
Shivangi Kamat ◽  
Sanket Deshpande ◽  
Lucky Kapoor ◽  
Dipankar Pal ◽  
Satyanarayana BHEESETTE
Keyword(s):  
High Altitude ◽  
Cosmic Ray ◽  
Cosmic Ray Flux
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