22-year variation pattern of cosmic ray intensity and solar activity
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概要
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It is well known that cosmic ray intensity variation present flat peak at sunspot minimum in one solar cycle (11year), and following next solar cycle present sharp peak at same phase of sunspot cycle. Flat peaks apear in positive state and sharp peaks in negative state. The relation between peak type of cosmic ray maximum and magnetic polarity pattern in heliosphere is a problem taken into account to reveal 22-year variation mechanism of cosmic ray intensity. To explain the peak pattern of 22-year cycle qualitatively, physical process can be presented in consideration of inward or outward motion of cosmic ray particle on the magnetic field structure of polarty pattern in heliosphere. In this paper, a simple process is proposed by introducing two factors, one is "capacity" of cosmic ray particles in heliocphere and the other is migration which changes trajectry of cosmic ray particles depending on the solar magnetic polarity (negative state or positive state). That is expected to make a contribution to understand the two type peak of cosmic ray intensity in the solar cycle dependence. Another problem is correlation with cosmic ray intensity and sunspot number which is established as inverse correlation. Indeed, maximum of cosmic ray intensity is well coincident with minimum of sunspot number, whereas minimum of cosmic ray intensity and corresponding maximum of sunspot number has some delay time of 1〜3 year. Especialy, time delay is long in odd cycle. Magnetic field structure of polarity pattern in heliosphere changes in odd or even cycle which affects propagation of cosmic ray.
- 松本大学の論文
- 2004-03-31
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