A new twist to the solar cycle

Details A new twist to the solar cycle A new twist to the solar cycle

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.247p...6c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 247, p. 6P-9P.

Astronomy and Astrophysics

Astronomy

8

Kelvin-Helmholtz Instability, Magnetic Flux, Solar Cycles, Solar Magnetic Field, Dynamo Theory, Magnetic Disturbances, Magnetic Field Configurations, Solar Convection (Astronomy)

Scientific paper

Recent numerical simulations of magnetic buoyancy instabilities suggest a new mechanism for the variation with the solar cycle in the scale and structure of surface magnetic flux. The nonlinear evolution of a predominantly toroidal field is found to depend crucially on the distribution of the weaker poloidal ingredient. For certain field configurations large, helical magnetic fragments are produced; for others the escaping field is small-scale and untwisted. We propose that the observed structural variations in flux may be accounted for by small changes in the twist of a deep-seated field. The large fragments will appear at the surface as active regions, which dominate at solar maximum, while the small-scale field will emerge as ephemeral regions which constitute practically all of the flux at solar minimum.

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