Abstract
In this chapter, we discuss what happens to a cosmic ray particle after it has successfully travelled through the heliosphere and the Earth’s magnetic field and has reached the top of the atmosphere. The fact that it made it so far means that its energy is high (≥1 GeV). Depending on the degree of solar activity (Sect. 5.7, also Fig. 10.2.3-1), the majority of the low energy particles fail to get close enough to the Earth to interact with matter even in the polar regions.
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Beer, J., McCracken, K., von Steiger, R. (2012). Production of Cosmogenic Radionuclides in the Atmosphere. In: Cosmogenic Radionuclides. Physics of Earth and Space Environments. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-14651-0_10
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DOI: https://doi.org/10.1007/978-3-642-14651-0_10
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