The structure of the global solar magnetic field excited by the turbulent dynamo mechanism

Details The structure of the global solar magnetic field excited by the turbulent dynamo mechanism The structure of the global solar magnetic field excited by the turbulent dynamo mechanism

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001arep...45..738k&link_type=abstract

Astronomy Reports, vol. 45, Issue 9, p.738-745

Astronomy and Astrophysics

Astronomy

1

Scientific paper

A mixing-length approximation is used to calculate Kλ for a Parker dynamo wave excited by the dynamo mechanism near the base of the solar convection zone (K is the wave number of the dynamo wave and λ the extent of the dynamo region). In a turbulent-dynamo model, this number characterizes the modes of the global magnetic field generated by a mechanism based on the joint action of the mean helical turbulence and solar differential rotation. Estimates are obtained for the helicity and radial angular-velocity gradient using the most recent helioseismological measurements at the growth phase of solar cycle 23. These estimates indicate that the dynamo mechanism most efficiently excites the fundamental antisymmetric (odd), dipole, mode of the poloidal field (Kλ≈-7) at low latitudes, while the conditions at latitudes above 50° are more favorable for the excitation of the lowest symmetric (even), quadrupole, mode (Kλ≈+8). The resulting north-south asymmetry of the poloidal field can explain the magnetic anomaly (“monopole” structure) of the polar fields observed near solar-cycle maxima. The effect of α quenching increases the calculated period of the dynamo-wave propagation from middle latitudes to the equator to about seven years, in rough agreement with the observed duration of the solar cycle.

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