Propagation of Galactic Cosmic Rays in the Heliosphere during Minimum Solar Activity Periods

Based on the cosmic ray transport equation, the propagation of charged high-energy particles in heliospheric magnetic fields is considered. The transport equation solution is found in the approximation of low anisotropy in the angular distribution of particles. The energy distribution of galactic co...

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Bibliographic Details
Published in:Kinematics and physics of celestial bodies 2024-04, Vol.40 (2), p.64-76
Main Author: Fedorov, Yu. I.
Format: Article
Language:English
Subjects:
Angular distribution
Anisotropy
Astronomy
Boundary conditions
Cosmic ray propagation
Cosmic ray showers
Cosmic rays
Energy distribution
Energy spectra
Flux density
Galactic cosmic rays
Heliopause
Heliosphere
Interplanetary magnetic field
Interstellar space
Magnetic fields
Observations and Techniques
Physics
Physics and Astronomy
Polarity
Solar activity
Space missions
Space Physics
Transport equations
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Summary:Based on the cosmic ray transport equation, the propagation of charged high-energy particles in heliospheric magnetic fields is considered. The transport equation solution is found in the approximation of low anisotropy in the angular distribution of particles. The energy distribution of galactic cosmic rays at a heliopause is used as a boundary condition. The energy spectrum of cosmic rays in a local interstellar space is considered to be known due to the outstanding results of space missions (Pioneer, Voyager, PAMELA, AMS-02, etc.). The flux density of cosmic rays is calculated in the periods of different solar magnetic polarity. It is shown that the intensity of galactic cosmic rays in positive magnetic polarity periods is maximum near the helioequator. In the periods when the interplanetary magnetic field has a negative polarity, the intensity of cosmic rays decreases with increasing heliolatitude.
ISSN:0884-5913
1934-8401
DOI:10.3103/S088459132402003X