Grand minima in a buoyancy-driven solar dynamo

Details Grand minima in a buoyancy-driven solar dynamo Grand minima in a buoyancy-driven solar dynamo

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...359..364o&link_type=abstract

Astronomy and Astrophysics, v.359, p.364-372 (2000)

Astronomy and Astrophysics

Astrophysics

15

Sun: Magnetic Fields, Sun: Activity, Magnetic Fields, Magnetohydrodynamics (Mhd)

Scientific paper

Numerical simulations of a 2D mean-field model are presented which show that grand minima, typical for the long-term behaviour of solar magnetic activity, can be produced by a dynamo that features an alpha effect based on the buoyancy instability of magnetic fluxtubes. The buoyancy-driven alpha effect functions only if the magnetic field strength exceeds a minimal value necessary for instability. It opens the possibility of dynamo action within the solar overshoot layer, where a strong magnetic field, B~ 105 G, is thought to be stored. The existence of a magnetic threshold for dynamo action can lead to interruptions of the magnetic cycle, similar to the grand minima of solar activity. Transitions across the instability threshold are triggered by magnetic-flux injections from the convection zone. This is modelled by allowing for a small-scale kinematic alpha effect in the convection zone, and convective downdrafts that penetrate the overshoot layer.

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