Physics
Scientific paper
Feb 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..191..247b&link_type=abstract
Solar Physics, v. 191, Issue 2, p. 247-255 (2000).
Physics
8
Scientific paper
Helicity of solar magnetic fields plays an important role in dynamo theories of the solar cycle. The helicity has been known to vary with the main 11-year period (Hale's cycle). Recent observations have revealed significant helicity variations on a shorter time scale, with a characteristic period of approximately 2 years. We suggest an explanation for the observed variations of the magnetic helicity, based on our model of the double magnetic cycle of solar activity. The quasi-biennial variations of the helicity are the consequence of the influence of erupted magnetic fields of the main cycle on the helicity in the regions of generation of the high-frequency component of magnetic field. This model suggests that the low-frequency component is generated at the base of the convective zone due to large-scale radial shear ∂Ω/∂r of angular velocity Ω. The high-frequency component may be generated in the subsurface region due to latitudinal shear ∂Ω/∂θ or due to the radial shear in this region.
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