Abstract
A numerical simulation of the global solar wind structure for Carrington rotation 1843 (31 May–28 June, 1991) is performed based on a fully three-dimensional, steady-state MHD model of the solar wind (Usmanov, 1993b). A self-consistent solution for 3-D MHD equations is constructed for the spherical shell extending from the solar photosphere up to 10 AU. Solar magnetic field observations are used to prescribe boundary conditions. The computed distribution of the magnetic field is compared with coronal hole observations and with the IMF measurements made by IMP-8 spacecraft at the Earth's orbit.
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References
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Usmanov, A.V. The global structure of the solar wind in June 1991. Sol Phys 148, 371–382 (1993). https://doi.org/10.1007/BF00645096
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DOI: https://doi.org/10.1007/BF00645096