We report on a study of the expected spatial variation of the galactic cosmic-ray intensity in the vicinity of the solar-wind termination shock. Model simulations predict that the radial gradients change abruptly at the shock, and that the nature of the effect varies significantly with particle energy. At low energies, the radial gradient changes abruptly from a lower value inside the shock to a higher value outside, whereas at high energies, the higher value of the gradient is inside the shock. This effect, which is a consequence of the matching conditions at the shock and is closely related to diffusive shock acceleration, is qualitatively the same for both heliospheric magnetic polarity states and remains much the same in one-dimensional, two-dimensional and three-dimensional models. Hence drifts do not change the nature of this phenomenon, although they change it quantitatively. The effect may prove to be an important diagnostic tool for the study of the termination of the solar wind.


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    Titel :

    Cosmic-ray gradients in the outer heliosphere


    Beteiligte:
    Kota, J. (Autor:in) / Jokipii, J. R. (Autor:in)

    Erschienen in:

    Erscheinungsdatum :

    1993-06-01



    Medientyp :

    Sonstige


    Format :

    Keine Angabe


    Sprache :

    Englisch


    Schlagwörter :


    Cosmic-Ray Gradients in the Outer Heliosphere

    Kota, J. | Online Contents | 1993


    Cosmic-ray gradients in the outer heliosphere

    Kóta, J. / Jokipii, J.R. | Elsevier | 1993


    Cosmic ray gradients in the heliosphere

    Fillius, Walker | NTRS | 1989


    Cosmic ray gradients in the heliosphere

    Fillius, Walker | Elsevier | 1989


    Cosmic Rays Transport in the Outer Heliosphere

    Valdes-Galicia, J.F. / Moussas, X. / Theodosiu, Z. et al. | Elsevier | 1993