Transport of cosmic rays in the solar corona | Zendy

L. A. Fisk | Zendy; Kenneth H. Schatten | Zendy

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Transport of cosmic rays in the solar corona

Author(s) -

L. A. Fisk,

Kenneth H. Schatten

Publication year - 1972

Publication title -

solar physics

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 1.026

H-Index - 123

eISSN - 1573-093X

pISSN - 0038-0938

DOI - 10.1007/bf00153904

Subject(s) - physics , corona (planetary geology) , cosmic ray , astrophysics , nanoflares , diffusion , photosphere , solar physics , classification of discontinuities , coronal radiative losses , magnetic field , computational physics , coronal mass ejection , solar wind , venus , mathematical analysis , mathematics , quantum mechanics , astrobiology , thermodynamics

A model is proposed to explain the transport of energetic protons in the solar corona. The particles are assumed to undergo an enhanced gradient-B drift along thin current sheets separating discontinuous field structures in the corona. These discontinuities may represent the extension into the corona of photospheric granular and supergranular cell boundaries. We have made a quantitative analysis of this process by assuming that the particle propagation can be described by a diffusion equation. Comparison of predictions of the model with cosmic ray observations at ~ 1 AU provide some support for the model.

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