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Description of galactic cosmic ray intensity in the last three solar activity minima

  • Proceedings of the 33rd National Conference on Cosmic Rays
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Bulletin of the Russian Academy of Sciences: Physics Aims and scope

Abstract

Using a numerical solution to the transport equation for galactic cosmic rays, the behavior of the intensity is described within a simple heliosphere model for the last three solar activity minima. The model differs from the ones we used earlier in the area of drift velocities, and in allowing for the difference between the characteristics of the heliospheric magnetic field inside and outside the sector zone. The results from calculations are compared with measurement data obtained for the intensity of galactic cosmic rays according to regular balloon monitoring in the Earth’s atmosphere.

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Authors and Affiliations

  1. Lebedev Physical Institute, Russian Academy of Sciences, Moscow, 119991, Russia

    M. S. Kalinin, G. A. Bazilevskaya, M. B. Krainev, N. S. Svirzhevsky, A. K. Svirzhevskaya & Y. I. Stozhkov

Authors
  1. M. S. Kalinin
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  2. G. A. Bazilevskaya
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  3. M. B. Krainev
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  4. N. S. Svirzhevsky
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  5. A. K. Svirzhevskaya
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  6. Y. I. Stozhkov
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Corresponding author

Correspondence to M. S. Kalinin.

Additional information

Original Russian Text © M.S. Kalinin, G.A. Bazilevskaya, M.B. Krainev, N.S. Svirzhevsky, A.K. Svirzhevskaya, Y.I. Stozhkov, 2015, published in Izvestiya Rossiiskoi Akademii Nauk. Seriya Fizicheskaya, 2015, Vol. 79, No. 5, pp. 660–662.

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Kalinin, M.S., Bazilevskaya, G.A., Krainev, M.B. et al. Description of galactic cosmic ray intensity in the last three solar activity minima. Bull. Russ. Acad. Sci. Phys. 79, 606–608 (2015). https://doi.org/10.3103/S1062873815050238

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  • DOI: https://doi.org/10.3103/S1062873815050238

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