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Properties of a cosmic ray flux crossing the magnetic cloud-solar wind interface

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

Abstract

A kinetic method for calculating cosmic ray propagation in a magnetic cloud is developed. The spatial distribution of cosmic rays and the residence time of particles of different energies inside the magnetic cloud are found. It is shown that any drop in the cosmic ray intensity inside a magnetic cloud is determined mainly by the geometry and the magnetic field strength.

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Authors and Affiliations

  1. Shafer Institute of Cosmophysical Research and Aeronomy, Siberian Branch, Russian Academy of Sciences, Yakutsk, 677980, Russia

    I. S. Petukhov & S. I. Petukhov

Authors
  1. I. S. Petukhov
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  2. S. I. Petukhov
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Corresponding author

Correspondence to I. S. Petukhov.

Additional information

Original Russian Text © I.S. Petukhov, S.I. Petukhov, 2015, published in Izvestiya Rossiiskoi Akademii Nauk. Seriya Fizicheskaya, 2015, Vol. 79, No. 5, pp. 694–696.

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Petukhov, I.S., Petukhov, S.I. Properties of a cosmic ray flux crossing the magnetic cloud-solar wind interface. Bull. Russ. Acad. Sci. Phys. 79, 640–642 (2015). https://doi.org/10.3103/S1062873815050354

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  • DOI: https://doi.org/10.3103/S1062873815050354

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