Meridional transport of magnetic flux in the solar wind between 1 and 10 AU - A theoretical analysis

Details Meridional transport of magnetic flux in the solar wind between 1 and 10 AU - A theoretical analysis Meridional transport of magnetic flux in the solar wind between 1 and 10 AU - A theoretical analysis

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....92.7241p&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 92, July 1, 1987, p. 7241-7253. NASA-supported research.

Astronomy and Astrophysics

Astronomy

20

Magnetic Flux, Meridional Flow, Solar Magnetic Field, Solar Wind, Astronomical Models, Interplanetary Magnetic Fields, Magnetohydrodynamics, Solar Cycles, Solar Flux

Scientific paper

Pioneer 10 observations suggest that the mean (longitudinally averaged) solar wind azimuthal field strength, Bφ, near the ecliptic plane falls off more rapidly with heliocentric distance than would be expected in a classic Parker expansion, showing a deficit of 10 - 20% (as compared to the projected 1-AU value) by 10 AU. Though this observational interpretation has been challenged by subsequent analyses of Voyager data, it has nevertheless stimulated efforts to explain the inferred deficit on the basis of systematic north-south magnetic pressure gradients generated by the differential spiral wrapping of magnetic field lines in interplanetary space. The authors reexamine this issue from the theoretical perspective using a three-dimensional MHD nonlinear numerical model for steady, corotating flow.

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