Fifty years of studying the GCR intensity during inversion of heliospheric magnetic fields I. Observations
Author:
Krainev Mikhail12, Bazilevskaya Galina3, Kalinin Mikhail3, Mihaylov Vladimir4, Svirzhevskaya Albina3, Svirzhevsky Nikolay3
Affiliation:
1. Lebedev Physical Institute, RAS 2. Shandong Institute of Advanced Technology 3. P.N. Lebedev Physical Institute of RAS 4. Moscow Engineering-Physics Institute
Abstract
The effects of the 22-year variation of solar magnetic fields in the galactic cosmic ray (GCR) intensity were first observed and interpreted as manifestations of inversion of the high-latitude solar magnetic field in properties of heliospheric magnetic fields by the Lebedev Physical Institute team in 1973. Since then, these effects have been studied already for 50 years.
The situation with the heliospheric magnetic field is clear for periods of medium and low sunspot activity — the heliosphere consists of two unipolar “hemispheres” separated by a wavy global heliospheric current sheet and characterized by a general polarity A (unit quantity with the sign of the radial component of the heliospheric magnetic field in the northern hemisphere). Yet there is no consensus on what the inversion of the heliospheric magnetic field is and which effects in the GCR intensity are connected with this phenomenon.
In this article, we briefly formulate general concepts of the 22-year variation in characteristics of the Sun, heliosphere, and GCR intensity and discuss the observed effects in the GCR intensity, which we attribute to the heliospheric magnetic field reversal. Models for this phenomenon and the results of GCR intensity calculations with these models will be discussed in the next article.
Publisher
Infra-M Academic Publishing House
Subject
Space and Planetary Science,Atmospheric Science,Geophysics
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