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A global numerical 3-D MHD model of the solar wind

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Abstract

A fully three-dimensional, steady-state global model of the solar corona and the solar wind is developed. A numerical, self-consistent solution for 3-D MHD equations is constructed for the region between the solar photosphere and the Earth's orbit. Boundary conditions are provided by the solar magnetic field observations. A steady-state solution is sought as a temporal relaxation to the dynamic equilibrium in the region of transonic flow near the Sun and then traced to the orbit of the Earth in supersonic flow region. The unique features of the proposed model are: (a) uniform coverage and self-consistent treatment of the regions of subsonic/sub-Alfvénic and supersonic/super-Alfvénic flows, (b) inferring the global structure of the interplanetary medium between the solar photosphere and 1 AU based on large-scale solar magnetic field data. As an experimental test for the proposed technique, photospheric magnetic field data for CR 1682 are used to prescribe boundary condition near the Sun and results of a simulation are compared with spacecraft measurements at 1 AU. The comparison demonstrates a qualitative agreement between computed and observed parameters. While the difference in densities is still significant, the 3-D model better reproduces variations of the solar wind velocity than does the 2-D model presented earlier (Usmanov, 1993).

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Authors and Affiliations

  1. Institute of Physics, University of St. Petersburg, 198904, St. Petersburg, Russia

    A. V. Usmanov

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  1. A. V. Usmanov
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Usmanov, A.V. A global numerical 3-D MHD model of the solar wind. Sol Phys 146, 377–396 (1993). https://doi.org/10.1007/BF00662021

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  • DOI: https://doi.org/10.1007/BF00662021

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