Simulations of the sun's polar magnetic fields during sunspot cycle 21

Details Simulations of the sun's polar magnetic fields during sunspot cycle 21 Simulations of the sun's polar magnetic fields during sunspot cycle 21

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..108...47d&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 108, no. 1, 1987, p. 47-59. Navy-supported research.

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46

Bipolarity, Line Of Sight, Polar Caps, Solar Magnetic Field, Solar Simulation, Sunspot Cycle, Computational Fluid Dynamics, Magnetic Flux, Meridional Flow, Polar Regions

Scientific paper

Regarding new bipolar magnetic regions as sources of flux, the evolution of the radial component of the solar photospheric magnetic field is simulated during 1976-1984, and the corresponding evolution of the line-of-sight polar fields as seen from earth is derived. The observed timing and strength of the polar-field reversal during cycle 21 can be accounted for by supergranular diffusion alone, for a diffusion coefficient of 800 sq km/sec. For an assumed 300 sq km/sec rate of diffusion, on the other hand, a poleward meridional flow with a moderately broad profile and a peak speed of 10 m/s reached at about 5 deg latitude is required to obtain agreement between the simulated and observed fields. Such a flow accelerates the transport of following-polarity flux to the polar caps, but also inhibits the diffusion of leading-polarity flux across the equator. For flows faster than about 10 m/s, the latter effect dominates, and the simulated polar fields reverse increasingly later and more weakly than the observed fields.

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