Magnetic rigidity dependence of eleven-year variation in cosmic ray intensity

1964 ◽  
Vol 69 (21) ◽  
pp. 4429-4434 ◽  
Author(s):  
T. Mathews ◽  
M. Kodama
Keyword(s):  
Cosmic Ray ◽  
Cosmic Ray Intensity ◽  
Magnetic Rigidity ◽  
Rigidity Dependence

The daily-variation second harmonic and a cosmic-ray intensity gradient perpendicular to the ecliptic

1968 ◽  
Vol 46 (10) ◽  
pp. S942-S945 ◽  
Author(s):  
B. Lietti ◽  
J. J. Quenby
Keyword(s):  
Daily Variation ◽  
Second Harmonic ◽  
Cosmic Ray ◽  
Ecliptic Plane ◽  
Positive Power ◽  
Cosmic Ray Intensity ◽  
Parallel Diffusion ◽  
Ray Density ◽  
Field Lines ◽  
Rigidity Dependence

Since the spiral interplanetary magnetic field is expected to be much less tightly wound at high solar latitudes, galactic particles arriving along the sun's polar field lines may suffer much less modulation than those arriving in the ecliptic plane. Hence a rising cosmic-ray density gradient is expected away from the ecliptic which will give rise to a second harmonic in the cosmic-ray daily variation with maxima at right angles to the spiral field direction. Two extreme models for the gradient are considered: one for predominantly particle diffusion along the field lines and the other when the diffusion is all perpendicular to the lines. Both models give a first positive power of rigidity dependence to the second harmonic in the 1 to 15 GV range with a double amplitude of about 0.05% at 10 GV. This is in rough accord with experimental results, which also can be shown to favor the parallel diffusion model at higher rigidities.

Rigidity dependence and the correlation with solar activity of the 11-year variation

1968 ◽  
Vol 46 (10) ◽  
pp. S915-S919 ◽  
Author(s):  
C. J. Hatton ◽  
P. L. Marsden ◽  
A. C. Willetts
Keyword(s):  
Solar Activity ◽  
Cosmic Ray ◽  
Phase Lag ◽  
Coronal Line ◽  
Cosmic Ray Intensity ◽  
Rigidity Dependence

The rigidity dependence of the modulation of the cosmic-ray intensity has been investigated using ground-based recorders during the period 1960–66. The intensities recorded by stations are found to be consistent with modulation spectra of the form (1−K/P and exp(−K/P) during the periods of increasing and decreasing cosmic-ray intensity. The question of the apparent phase lag of the cosmic-ray intensity behind the solar activity has also been examined. It is shown that the cosmic-ray intensity is well correlated with the emission of the coronal line, λ5303, from the vicinity of the solar equator.

scholarly journals Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

2019 ◽  
Vol 209 ◽  
pp. 01007
Author(s):  
Francesco Nozzoli
Keyword(s):  
Electron Flux ◽  
Space Station ◽  
Cosmic Ray ◽  
High Energy ◽  
Precision Measurements ◽  
High Energy Electrons ◽  
Electrons And Positrons ◽  
Positron Flux ◽  
Rigidity Dependence ◽  
Alpha Magnetic Spectrometer

Precision measurements by AMS of the fluxes of cosmic ray positrons, electrons, antiprotons, protons as well as their rations reveal several unexpected and intriguing features. The presented measurements extend the energy range of the previous observations with much increased precision. The new results show that the behavior of positron flux at around 300 GeV is consistent with a new source that produce equal amount of high energy electrons and positrons. In addition, in the absolute rigidity range 60–500 GV, the antiproton, proton, and positron fluxes are found to have nearly identical rigidity dependence and the electron flux exhibits different rigidity dependence.

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